Astronomy:Globular cluster

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Short description: Spherical collection of stars

Template:Infobox astronomical formation A globular cluster is a spheroidal conglomeration of stars that is bound together by gravity, with a higher concentration of stars towards their centers. They can contain anywhere from tens of thousands to many millions of member stars,[1] all orbiting in a stable, compact formation. Globular clusters are similar in form to dwarf spheroidal galaxies, and the distinction between the two is not always clear.[2] Their name is derived from Latin globulus (small sphere). Globular clusters are occasionally known simply as "globulars".

Although one globular cluster, Omega Centauri, was observed in antiquity and long thought to be a star, recognition of the clusters' true nature came with the advent of telescopes in the 17th century. In early telescopic observations globular clusters appeared as fuzzy blobs, leading French astronomer Charles Messier to include many of them in his catalog of astronomical objects that he thought could be mistaken for comets. Using larger telescopes, 18th-century astronomers recognized that globular clusters are groups of many individual stars. Early in the 20th century the distribution of globular clusters in the sky was some of the first evidence that the Sun is far from the center of the Milky Way.

Globular clusters are found in nearly all galaxies. In spiral galaxies like the Milky Way they are mostly found in the outer spheroidal part of the galaxy – the galactic halo. They are the largest and most massive type of star cluster, tending to be older, denser, and composed of lower abundances of heavy elements than open clusters, which are generally found in the disks of spiral galaxies. The Milky Way has more than 150 known globulars, and there may be many more.

The origin of globular clusters and their role in galactic evolution are unclear. Some are among the oldest objects in their galaxies and even the universe, constraining estimates of the universe's age. Star clusters were formerly thought to consist of stars that all formed at the same time from one star-forming nebula, but nearly all globular clusters contain stars that formed at different times, or that have differing compositions. Some clusters may have had multiple episodes of star formation, and some may be remnants of smaller galaxies captured by larger galaxies.

History of observations

The first known globular cluster, now called M 22, was discovered in 1665 by Abraham Ihle, a German amateur astronomer.[3][4] The cluster Omega Centauri, easily visible in the southern sky with the naked eye, was known to ancient astronomers like Ptolemy as a star, but was reclassified as a nebula by Edmond Halley in 1677, then finally as a globular cluster in the early 19th century by John Herschel.[5][6] The French astronomer Abbé Lacaille listed NGC 104, NGC 4833, M 55, M 69, and NGC 6397 in his 1751–1752 catalogue.[lower-alpha 1] The low resolution of early telescopes prevented individual stars in a cluster from being visually separated until Charles Messier observed M 4 in 1764.[7][lower-alpha 2][8]

Early globular cluster discoveries
Cluster name Discovered by Year
M 22[3] Abraham Ihle 1665
Edmond Halley 1677
Gottfried Kirch 1702
M 13[9](p 235) Edmond Halley 1714
M 71[10] Philippe Loys de Chéseaux 1745
M 4[10] Philippe Loys de Chéseaux 1746
M 15[11] Jean-Dominique Maraldi 1746
M 2[11] Jean-Dominique Maraldi 1746

When William Herschel began his comprehensive survey of the sky using large telescopes in 1782, there were 34 known globular clusters. Herschel discovered another 36 and was the first to resolve virtually all of them into stars. He coined the term globular cluster in his Catalogue of a Second Thousand New Nebulae and Clusters of Stars (1789).[12][lower-alpha 3][13] In 1914 Harlow Shapley began a series of studies of globular clusters, published across about forty scientific papers. He examined the clusters' RR Lyrae variables (stars which he assumed were Cepheid variables) and used their luminosity and period of variability to estimate the distances to the clusters. It was later found that RR Lyrae variables are fainter than Cepheid variables, causing Shapley to overestimate the distances.[14]

Thousands of white-ish dots scattered on a black background, strongly concentrated towards the center
NGC 7006 is a highly concentrated, Class I globular cluster.

A large majority of the Milky Way's globular clusters are found around the galactic core. In 1918 Shapley used this strongly asymmetrical distribution to determine the overall dimensions of the galaxy. Assuming a roughly spherical distribution of globular clusters around the galaxy's center, he used the positions of the clusters to estimate the position of the Sun relative to the Galactic Center.[15] He correctly concluded that the Milky Way's center is in the Sagittarius constellation and not near the Earth. He overestimated the distance, finding typical globular cluster distances of 10–30 kiloparsecs (33,000–98,000 ly);[16] the modern distance to the Galactic Center is roughly 8.5 kiloparsecs (28,000 ly).[lower-alpha 4][17][18][19] Shapley's measurements indicated the Sun is relatively far from the center of the galaxy, contrary to what had been inferred from the observed uniform distribution of ordinary stars. In reality most ordinary stars lie within the galaxy's disk and are thus obscured by gas and dust in the disk, whereas globular clusters lie outside the disk and can be seen at much greater distances.[14]

Thousands of white-ish dots scattered on a black background, strongly concentrated towards the center
The Messier 80 globular cluster in the constellation Scorpius is located about 30,000 light-years from the Sun and contains hundreds of thousands of stars.[20]

The count of known globular clusters in the Milky Way has continued to increase, reaching 83 in 1915, 93 in 1930, 97 by 1947,[13] and 157 in 2010.[21][22] Additional, undiscovered globular clusters are believed to be in the galactic bulge[23] or hidden by the gas and dust of the Milky Way.[24] For example, most of the Palomar Globular Clusters have only been discovered in the 1950s, with some located relatively close-by yet obscured by dust, while others reside in the very far reaches of the Milky Way halo. The Andromeda Galaxy, which is comparable in size to the Milky Way, may have as many as five hundred globulars.[25] Every galaxy of sufficient mass in the Local Group has an associated system of globular clusters, as does almost every large galaxy surveyed.[26] Some giant elliptical galaxies (particularly those at the centers of galaxy clusters), such as M 87, have as many as 13,000 globular clusters.[27]

Classification

Main page: Shapley–Sawyer Concentration Class

Shapley was later assisted in his studies of clusters by Henrietta Swope and Helen Sawyer Hogg. In 1927–1929 Shapley and Sawyer categorized clusters by the degree of concentration of stars toward each core. Their system, known as the Shapley–Sawyer Concentration Class, identifies the most concentrated clusters as Class I and ranges to the most diffuse Class XII.[lower-alpha 5][28] In 2015 astronomers from the Pontifical Catholic University of Chile proposed a new type of globular cluster on the basis of observational data: Dark globular clusters.[29]

Formation

Thousands of white-ish dots scattered on a black background, strongly concentrated towards the center
NGC 2808 contains three distinct generations of stars.[30]
NASA image

The formation of globular clusters is poorly understood.[31] Globular clusters have traditionally been described as a simple star population formed from a single giant molecular cloud, and thus with roughly uniform age and metallicity (proportion of heavy elements in their composition). Modern observations show that nearly all globular clusters contain multiple populations;[32] the globular clusters in the Large Magellanic Cloud (LMC) exhibit a bimodal population, for example. During their youth, these LMC clusters may have encountered giant molecular clouds that triggered a second round of star formation.[33] This star-forming period is relatively brief, compared with the age of many globular clusters.[34] It has been proposed that this multiplicity in stellar populations could have a dynamical origin. In the Antennae Galaxy, for example, the Hubble Space Telescope has observed clusters of clusters – regions in the galaxy that span hundreds of parsecs, in which many of the clusters will eventually collide and merge. Their overall range of ages and (possibly) metallicities could lead to clusters with a bimodal, or even multiple, distribution of populations.[35]

A small fuzzy white ball in the center of a speckled black backdrop
Globular star cluster Messier 54[36]

Observations of globular clusters show that their stars primarily come from regions of more efficient star formation, and from where the interstellar medium is at a higher density, as compared to normal star-forming regions. Globular cluster formation is prevalent in starburst regions and in interacting galaxies.[37] Some globular clusters likely formed in dwarf galaxies and were removed by tidal forces to join the Milky Way.[38] In elliptical and lenticular galaxies there is a correlation between the mass of the supermassive black holes (SMBHs) at their centers and the extent of their globular cluster systems. The mass of the SMBH in such a galaxy is often close to the combined mass of the galaxy's globular clusters.[39]

No known globular clusters display active star formation, consistent with the hypothesis that globular clusters are typically the oldest objects in their galaxy and were among the first collections of stars to form. Very large regions of star formation known as super star clusters, such as Westerlund 1 in the Milky Way, may be the precursors of globular clusters.[40]

Many of the Milky Way's globular clusters have a retrograde orbit (meaning that they revolve around the galaxy in the reverse of the direction the galaxy is rotating),[41] including the most massive, Omega Centauri. Its retrograde orbit suggests it may be a remnant of a dwarf galaxy captured by the Milky Way.[42][43]

Composition

A loose scattering of small dull white dots on a black background with a few brighter coloured stars
Djorgovski 1's stars contain hydrogen and helium, but not much else. In astronomical terms they are metal-poor.[44]

Globular clusters are generally composed of hundreds of thousands of low-metal, old stars. The stars found in a globular cluster are similar to those in the bulge of a spiral galaxy but confined to a spheroid in which half the light is emitted within a radius of only a few to a few tens of parsecs.[31] They are free of gas and dust[45] and it is presumed that all the gas and dust was long ago either turned into stars or blown out of the cluster by the massive first-generation stars.[31]

Globular clusters can contain a high density of stars; on average about 0.4 stars per cubic parsec, increasing to 100 or 1000 stars/pc3 in the core of the cluster.[46] In comparison, the stellar density around the Sun is roughly 0.1 stars/pc3.[47] The typical distance between stars in a globular cluster is about one light year,[48] but at its core the separation between stars averages about a third of a light year – thirteen times closer than the Sun is to its nearest neighbor, Proxima Centauri.[49]

Globular clusters are thought to be unfavorable locations for planetary systems. Planetary orbits are dynamically unstable within the cores of dense clusters because of the gravitational perturbations of passing stars. A planet orbiting at one astronomical unit around a star that is within the core of a dense cluster, such as 47 Tucanae, would survive only on the order of a hundred million years.[50] There is a planetary system orbiting a pulsar (PSR B1620−26) that belongs to the globular cluster M4, but these planets likely formed after the event that created the pulsar.[51]

Some globular clusters, like Omega Centauri in the Milky Way and Mayall II in the Andromeda Galaxy, are extraordinarily massive, measuring several million solar masses (M☉) and having multiple stellar populations. Both are evidence that supermassive globular clusters formed from the cores of dwarf galaxies that have been consumed by larger galaxies.[52] About a quarter of the globular cluster population in the Milky Way may have been accreted this way,[53] as with more than 60% of the globular clusters in the outer halo of Andromeda.[54]

Heavy element content

Globular clusters normally consist of Population II stars which, compared with Population I stars such as the Sun, have a higher proportion of hydrogen and helium and a lower proportion of heavier elements. Astronomers refer to these heavier elements as metals (distinct from the material concept) and to the proportions of these elements as the metallicity. Produced by stellar nucleosynthesis, the metals are recycled into the interstellar medium and enter a new generation of stars. The proportion of metals can thus be an indication of the age of a star in simple models, with older stars typically having a lower metallicity.[55]

The Dutch astronomer Pieter Oosterhoff observed two special populations of globular clusters, which became known as Oosterhoff groups. The second group has a slightly longer period of RR Lyrae variable stars.[56] While both groups have a low proportion of metallic elements as measured by spectroscopy, the metal spectral lines in the stars of Oosterhoff type I (Oo I) cluster are not quite as weak as those in type II (Oo II),[56] and so type I stars are referred to as metal-rich (e.g. Terzan 7[57]), while type II stars are metal-poor (e.g. ESO 280-SC06[58]). These two distinct populations have been observed in many galaxies, especially massive elliptical galaxies. Both groups are nearly as old as the universe itself and are of similar ages. Suggested scenarios to explain these subpopulations include violent gas-rich galaxy mergers, the accretion of dwarf galaxies, and multiple phases of star formation in a single galaxy. In the Milky Way the metal-poor clusters are associated with the halo and the metal-rich clusters with the bulge.[59]

In the Milky Way a large majority of the metal-poor clusters are aligned on a plane in the outer part of the galaxy's halo. This observation supports the view that type II clusters were captured from a satellite galaxy, rather than being the oldest members of the Milky Way's globular cluster system as was previously thought. The difference between the two cluster types would then be explained by a time delay between when the two galaxies formed their cluster systems.[60]

Exotic components

Thousands of white-ish dots scattered on a black background, strongly concentrated towards the center
Messier 53 contains an unusually large number of a type of star called blue stragglers.[61][62]

Close interactions and near-collisions of stars occur relatively often in globular clusters because of their high star density. These chance encounters give rise to some exotic classes of stars – such as blue stragglers, millisecond pulsars, and low-mass X-ray binaries – which are much more common in globular clusters. How blue stragglers form remains unclear, but most models attribute them to interactions between stars, such as stellar mergers, the transfer of material from one star to another, or even an encounter between two binary systems.Cite error: Closing </ref> missing for <ref> tag but this claim is contested.[63]]]

Simulation of stellar motions in Messier 4
Simulation of stellar motions in Messier 4, where astronomers suspect that an intermediate-mass black hole could be present.[64][65] If confirmed, the black hole would be in the center of the cluster, and would have a sphere of influence (black hole) limited by the red circle.

Astronomers have searched for black holes within globular clusters since the 1970s. The required resolution for this task is exacting; it is only with the Hubble Space Telescope (HST) that the first claimed discoveries were made, in 2002 and 2003. Based on HST observations, other researchers suggested the existence of a 4,000 M☉(solar masses) intermediate-mass black hole in the globular cluster M15 and a 20,000 M☉ black hole in the Mayall II cluster of the Andromeda Galaxy.[66] Both X-ray and radio emissions from Mayall II appear consistent with an intermediate-mass black hole;[67] however, these claimed detections are controversial.[68]

The heaviest objects in globular clusters are expected to migrate to the cluster center due to mass segregation. One research group pointed out that the mass-to-light ratio should rise sharply towards the center of the cluster, even without a black hole, in both M15[63] and Mayall II.[69] Observations from 2018 find no evidence for an intermediate-mass black hole in any globular cluster, including M15, but cannot definitively rule out one with a mass of 500–1000 M☉.[70] Finally, in 2023, an analysis of HST and the Gaia spacecraft data from the closest globular cluster, Messier 4, revealed an excess mass of roughly 800 M☉ in the center of this cluster, which appears to not be extended. This could thus be the best kinematic evidence for an intermediate-mass black hole[64][65] (even if an unusually compact cluster of compact objects like white dwarfs, neutron stars or stellar-mass black holes cannot be completely discounted).

The confirmation of intermediate-mass black holes in globular clusters would have important ramifications for theories of galaxy development as being possible sources for the supermassive black holes at their centers. The mass of these supposed intermediate-mass black holes is proportional to the mass of their surrounding clusters, following a pattern previously discovered between supermassive black holes and their surrounding galaxies.[68][71]

Hertzsprung–Russell diagrams

A scattering of dots on a black background, most yellow and aligned in a roughly vertical band down the center, with some white dots extending in two arms to the left and a few red dots scattered on the right of the image
H–R diagram for the globular cluster M3. There is a characteristic "knee" in the curve at magnitude 19 where stars begin entering the giant stage of their evolutionary path, the main-sequence turnoff.

Hertzsprung–Russell diagrams (H–R diagrams) of globular clusters allow astronomers to determine many of the properties of their populations of stars. An H–R diagram is a graph of a large sample of stars plotting their absolute magnitude (their luminosity, or brightness measured from a standard distance), as a function of their color index. The color index, roughly speaking, measures the color of the star; positive color indices indicate a reddish star with a cool surface temperature, while negative values indicate a bluer star with a hotter surface. Stars on an H–R diagram mostly lie along a roughly diagonal line sloping from hot, luminous stars in the upper left to cool, faint stars in the lower right. This line is known as the main sequence and represents the primary stage of stellar evolution. The diagram also includes stars in later evolutionary stages such as the cool but luminous red giants.[72]

Constructing an H–R diagram requires knowing the distance to the observed stars to convert apparent into absolute magnitude. Because all the stars in a globular cluster have about the same distance from Earth, a color–magnitude diagram using their observed magnitudes looks like a shifted H–R diagram (because of the roughly constant difference between their apparent and absolute magnitudes).[73] This shift is called the distance modulus and can be used to calculate the distance to the cluster. The modulus is determined by comparing features (like the main sequence) of the cluster's color–magnitude diagram to corresponding features in an H–R diagram of another set of stars, a method known as spectroscopic parallax or main-sequence fitting.[74]

Properties

Since globular clusters form at once from a single giant molecular cloud, a cluster's stars have roughly the same age and composition. A star's evolution is primarily determined by its initial mass, so the positions of stars in a cluster's H–R or color–magnitude diagram mostly reflect their initial masses. A cluster's H–R diagram, therefore, appears quite different from H–R diagrams containing stars of a wide variety of ages. Almost all stars fall on a well-defined curve in globular cluster H–R diagrams, and that curve's shape indicates the age of the cluster.[73][75] A more detailed H–R diagram often reveals multiple stellar populations as indicated by the presence of closely separated curves, each corresponding to a distinct population of stars with a slightly different age or composition.[32] Observations with the Wide Field Camera 3, installed in 2009 on the Hubble Space Telescope, made it possible to distinguish these slightly different curves.[76]

The most massive main-sequence stars have the highest luminosity and will be the first to evolve into the giant star stage. As the cluster ages, stars of successively lower masses will do the same. Therefore, the age of a single-population cluster can be measured by looking for those stars just beginning to enter the giant star stage, which form a "knee" in the H–R diagram called the main-sequence turnoff, bending to the upper right from the main-sequence line. The absolute magnitude at this bend is directly a function of the cluster's age; an age scale can be plotted on an axis parallel to the magnitude.[73]

The morphology and luminosity of globular cluster stars in H–R diagrams are influenced by numerous parameters, many of which are still actively researched. Recent observations have overturned the historical paradigm that all globular clusters consist of stars born at exactly the same time, or sharing exactly the same chemical abundance. Some clusters feature multiple populations, slightly differing in composition and age; for example, high-precision imagery of cluster NGC 2808 discerned three close, but distinct, main sequences.[77] Further, the placements of the cluster stars in an H–R diagram (including the brightnesses of distance indicators) can be influenced by observational biases. One such effect, called blending, arises when the cores of globular clusters are so dense that observations see multiple stars as a single target. The brightness measured for that seemingly single star is thus incorrect – too bright, given that multiple stars contributed.[78] The computed distance is in turn incorrect, so the blending effect can introduce a systematic uncertainty into the cosmic distance ladder and may bias the estimated age of the universe and the Hubble constant.[79]

Consequences

The blue stragglers appear on the H–R diagram as a series diverging from the main sequence in the direction of brighter, bluer stars.[80] White dwarfs (the final remnants of some Sun-like stars), which are much fainter and somewhat hotter than the main-sequence stars, lie on the bottom-left of an H–R diagram. Globular clusters can be dated by looking at the temperatures of the coolest white dwarfs, often giving results as old as 12.7 billion years.[81] In comparison, open clusters are rarely older than about half a billion years.[82] The ages of globular clusters place a lower bound on the age of the entire universe, presenting a significant constraint in cosmology. Astronomers were historically faced with age estimates of clusters older than their cosmological models would allow,[83] but better measurements of cosmological parameters, through deep sky surveys and satellites, appear to have resolved this issue.[84][85]

Studying globular clusters sheds light on how the composition of the formational gas and dust affects stellar evolution; the stars' evolutionary tracks vary depending on the abundance of heavy elements. Data obtained from these studies are then used to study the evolution of the Milky Way as a whole.[86]

Morphology

Ellipticity of globular clusters
Galaxy Ellipticity[87]
Milky Way 0.07±0.04
LMC 0.16±0.05
SMC 0.19±0.06
M31 0.09±0.04

In contrast to open clusters, most globular clusters remain gravitationally bound together for time periods comparable to the lifespans of most of their stars. Strong tidal interactions with other large masses result in the dispersal of some stars, leaving behind "tidal tails" of stars removed from the cluster.[88][89]

After formation, the stars in the globular cluster begin to interact gravitationally with each other. The velocities of the stars steadily change, and the stars lose any history of their original velocity. The characteristic interval for this to occur is the relaxation time, related to the characteristic length of time a star needs to cross the cluster and the number of stellar masses.[90] The relaxation time varies by cluster, but a typical value is on the order of one billion years.[91][92]

Although globular clusters are generally spherical in form, ellipticity can form via tidal interactions. Clusters within the Milky Way and the Andromeda Galaxy are typically oblate spheroids in shape, while those in the Large Magellanic Cloud are more elliptical.[93]

Radii

Hundreds of white-ish dots scattered on a black background, concentrated towards the center, with some brighter red and blue dots scattered across the frame
NGC 411 is classified as an open cluster.[94]

Astronomers characterize the morphology (shape) of a globular cluster by means of standard radii: the core radius (rc), the half-light radius (rh), and the tidal or Jacobi radius (rt). The radius can be expressed as a physical distance or as a subtended angle in the sky. Considering a radius around the core, the surface luminosity of the cluster steadily decreases with distance, and the core radius is the distance at which the apparent surface luminosity has dropped by half.[95] A comparable quantity is the half-light radius, or the distance from the core containing half the total luminosity of the cluster; the half-light radius is typically larger than the core radius.[96][97]

Most globular clusters have a half-light radius of less than ten parsecs (pc), although some globular clusters have very large radii, like NGC 2419 (rh = 18 pc) and Palomar 14 (rh = 25 pc).[98] The half-light radius includes stars in the outer part of the cluster that happen to lie along the line of sight, so theorists also use the half-mass radius (rm) – the radius from the core that contains half the total mass of the cluster. A small half-mass radius, relative to the overall size, indicates a dense core. Messier 3 (M3), for example, has an overall visible dimension of about 18 arc minutes, but a half-mass radius of only 1.12 arc minutes.[99]

The tidal radius, or Hill sphere, is the distance from the center of the globular cluster at which the external gravitation of the galaxy has more influence over the stars in the cluster than does the cluster itself.[100] This is the distance at which the individual stars belonging to a cluster can be separated away by the galaxy. The tidal radius of M3, for example, is about forty arc minutes,[101] or about 113 pc.[102]

Mass segregation, luminosity and core collapse

In most Milky Way clusters the surface brightness of a globular cluster as a function of decreasing distance to the core first increases, then levels off at a distance typically 1–2 parsecs from the core. About 20% of the globular clusters have undergone a process termed "core collapse". In such a cluster the luminosity increases steadily all the way to the core region.[103][104]

Thousands of white-ish dots scattered on a black background, strongly concentrated towards the center
47 Tucanae is the second most luminous globular cluster in the Milky Way, after Omega Centauri.

Models of globular clusters predict core collapse occurs when the more massive stars in a globular cluster encounter their less massive counterparts. Over time, dynamic processes cause individual stars to migrate from the center of the cluster to the outside, resulting in a net loss of kinetic energy from the core region and leading the region's remaining stars to occupy a more compact volume. When this gravothermal instability occurs, the central region of the cluster becomes densely crowded with stars, and the surface brightness of the cluster forms a power-law cusp.[105] A massive black hole at the core could also result in a luminosity cusp.[106] Over a long time this leads to a concentration of massive stars near the core, a phenomenon called mass segregation.[107]

The dynamical heating effect of binary star systems works to prevent an initial core collapse of the cluster. When a star passes near a binary system, the orbit of the latter pair tends to contract, releasing energy. Only after this primordial supply of energy is exhausted can a deeper core collapse proceed.[108][109] In contrast, the effect of tidal shocks as a globular cluster repeatedly passes through the plane of a spiral galaxy tends to significantly accelerate core collapse.[110]

Core collapse may be divided into three phases. During a cluster's adolescence, core collapse begins with stars nearest the core. Interactions between binary star systems prevents further collapse as the cluster approaches middle age. The central binaries are either disrupted or ejected, resulting in a tighter concentration at the core.[111] The interaction of stars in the collapsed core region causes tight binary systems to form. As other stars interact with these tight binaries they increase the energy at the core, causing the cluster to re-expand. As the average time for a core collapse is typically less than the age of the galaxy, many of a galaxy's globular clusters may have passed through a core collapse stage, then re-expanded.[112]

Hundreds of white-ish dots scattered on a black background, concentrated towards the center
Globular cluster NGC 1854 is located in the Large Magellanic Cloud.[113]

The HST has provided convincing observational evidence of this stellar mass-sorting process in globular clusters. Heavier stars slow down and crowd at the cluster's core, while lighter stars pick up speed and tend to spend more time at the cluster's periphery. The cluster 47 Tucanae, made up of about one million stars, is one of the densest globular clusters in the Southern Hemisphere. This cluster was subjected to an intensive photographic survey that obtained precise velocities for nearly fifteen thousand stars in this cluster.[114]

The overall luminosities of the globular clusters within the Milky Way and the Andromeda Galaxy each have a roughly Gaussian distribution, with an average magnitude Mv and a variance σ2. This distribution of globular cluster luminosities is called the Globular Cluster Luminosity Function (GCLF). For the Milky Way, Mv = −7.29 ± 0.13, σ = 1.1 ± 0.1. The GCLF has been used as a "standard candle" for measuring the distance to other galaxies, under the assumption that globular clusters in remote galaxies behave similarly to those in the Milky Way.[115]

N-body simulations

Main page: Physics:N-body simulation

Computing the gravitational interactions between stars within a globular cluster requires solving the N-body problem. The naive computational cost for a dynamic simulation increases in proportion to N 2 (where N is the number of objects), so the computing requirements to accurately simulate a cluster of thousands of stars can be enormous.[116][117] A more efficient method of simulating the N-body dynamics of a globular cluster is done by subdivision into small volumes and velocity ranges, and using probabilities to describe the locations of the stars. Their motions are described by means of the Fokker–Planck equation, often using a model describing the mass density as a function of radius, such as a Plummer model. The simulation becomes more difficult when the effects of binaries and the interaction with external gravitation forces (such as from the Milky Way galaxy) must also be included.[118] In 2010 a low-density globular cluster's lifetime evolution was able to be directly computed, star-by-star.[119]

Completed N-body simulations have shown that stars can follow unusual paths through the cluster, often forming loops and falling more directly toward the core than would a single star orbiting a central mass. Additionally, some stars gain sufficient energy to escape the cluster due to gravitational interactions that result in a sufficient increase in velocity. Over long periods of time this process leads to the dissipation of the cluster, a process termed evaporation.[120] The typical time scale for the evaporation of a globular cluster is 1010 years.[90] The ultimate fate of a globular cluster must be either to accrete stars at its core, causing its steady contraction,[121] or gradual shedding of stars from its outer layers.[122]

Binary stars form a significant portion of stellar systems, with up to half of all field stars and open cluster stars occurring in binary systems.[123][124] The present-day binary fraction in globular clusters is difficult to measure, and any information about their initial binary fraction is lost by subsequent dynamical evolution.[125] Numerical simulations of globular clusters have demonstrated that binaries can hinder and even reverse the process of core collapse in globular clusters. When a star in a cluster has a gravitational encounter with a binary system, a possible result is that the binary becomes more tightly bound and kinetic energy is added to the solitary star. When the massive stars in the cluster are sped up by this process, it reduces the contraction at the core and limits core collapse.[126][127]

Intermediate forms

Thousands of white-ish dots scattered on a black background, strongly concentrated towards the center
Messier 10 lies about 15,000 light-years from Earth, in the constellation of Ophiuchus.[128]

Cluster classification is not always definitive; objects have been found that can be classified in more than one categories. For example, BH 176 in the southern part of the Milky Way has properties of both an open and a globular cluster.[129]

In 2005 astronomers discovered a new, "extended" type of star cluster in the Andromeda Galaxy's halo, similar to the globular cluster. The three new-found clusters have a similar star count as globular clusters and share other characteristics, such as stellar populations and metallicity, but are distinguished by their larger size – several hundred light years across – and some hundred times lower density. Their stars are separated by larger distances; parametrically, these clusters lie somewhere between a globular cluster and a dwarf spheroidal galaxy.[130] The formation of these extended clusters is likely related to accretion.[131] It is unclear why the Milky Way lacks such clusters; Andromeda is unlikely to be the sole galaxy with them, but their presence in other galaxies remains unknown.[130]

Tidal encounters

When a globular cluster comes close to a large mass, such as the core region of a galaxy, it undergoes a tidal interaction. The difference in gravitational strength between the nearer and further parts of the cluster results in an asymmetric, tidal force. A "tidal shock" occurs whenever the orbit of a cluster takes it through the plane of a galaxy.[110][132]

Tidal shocks can pull stars away from the cluster halo, leaving only the core part of the cluster; these trails of stars can extend several degrees away from the cluster.[133] These tails typically both precede and follow the cluster along its orbit and can accumulate significant portions of the original mass of the cluster, forming clump-like features.[134] The globular cluster Palomar 5, for example, is near the apogalactic point of its orbit after passing through the Milky Way. Streams of stars extend outward toward the front and rear of the orbital path of this cluster, stretching to distances of 13,000 light years. Tidal interactions have stripped away much of Palomar 5's mass; further interactions with the galactic core are expected to transform it into a long stream of stars orbiting the Milky Way in its halo.[135]

The Milky Way is in the process of tidally stripping the Sagittarius Dwarf Spheroidal Galaxy of stars and globular clusters through the Sagittarius Stream. As many as 20% of the globular clusters in the Milky Way's outer halo may have originated in that galaxy.[136] Palomar 12, for example, most likely originated in the Sagittarius Dwarf Spheroidal but is now associated with the Milky Way.[137][138] Tidal interactions like these add kinetic energy into a globular cluster, dramatically increasing the evaporation rate and shrinking the size of the cluster.[90] The increased evaporation accelerates the process of core collapse.[90][139]

Planets

Astronomers are searching for exoplanets of stars in globular star clusters.[140] A search in 2000 for giant planets in the globular cluster 47 Tucanae came up negative, suggesting that the abundance of heavier elements – low in globular clusters – necessary to build these planets may need to be at least 40% of the Sun's abundance. Because terrestrial planets are built from heavier elements such as silicon, iron and magnesium, member stars have a far lower likelihood of hosting Earth-mass planets than stars in the solar neighborhood. Globular clusters are thus unlikely to host habitable terrestrial planets.[141]

A giant planet was found in the globular cluster Messier 4, orbiting a pulsar in the binary star system PSR B1620-26. The planet's eccentric and highly inclined orbit suggests it may have been formed around another star in the cluster, then "exchanged" into its current arrangement.[142] The likelihood of close encounters between stars in a globular cluster can disrupt planetary systems; some planets break free to become rogue planets, orbiting the galaxy. Planets orbiting close to their star can become disrupted, potentially leading to orbital decay and an increase in orbital eccentricity and tidal effects.[143]

See also

Footnotes

  1. ↑ The label M before a number refers to Charles Messier's catalogue, while NGC is from the New General Catalogue by John Dreyer.
  2. ↑ From page 437: Le 8 Mai 1764, j'ai découvert une nébuleuse ... de 25d 55′ 40″ méridionale.
    "On 8 May 1764, I discovered a nebula near Antares, and on its parallel; it is a [source of] light which has little extension, which is dim, and which is seen with difficulty; by using a good telescope to see it, one perceives very small stars in it. Its right ascension was determined to be 242° 16′ 56″, and its declination, 25° 55′ 40″ south."[7](p 437)
  3. ↑ From page 218, discussing the shapes of star clusters, Herschel wrote:
    "And thus, from the above-mentioned appearances, we come to know that there are globular clusters of stars nearly equal in size, which are scattered evenly at equal distances from the middle, but with an encreasing [sic] accumulation towards the center."[12](p 218)
  4. ↑ Harlow Shapley's error was aggravated by interstellar dust in the Milky Way, which absorbs and diminishes the amount of light from distant objects (such as globular clusters), thus making them appear to be farther away.
  5. ↑ The Concentration Class is sometimes given with Arabic numerals (Classes 1–12) rather than Roman numerals.

References

  1. ↑ "Globular cluster". https://esahubble.org/wordbank/globular-cluster/. 
  2. ↑ Van Den Bergh, Sidney (March 2008). "Globular clusters and dwarf spheroidal galaxies". Monthly Notices of the Royal Astronomical Society: Letters 385 (1): L20–L22. doi:10.1111/j.1745-3933.2008.00424.x. Bibcode: 2008MNRAS.385L..20V. 
  3. ↑ 3.0 3.1 Lynn, W.T. (April 1886). "The discovery of the star-cluster 22 Messier in Sagittarius". The Observatory 9: 163–164. Bibcode: 1886Obs.....9..163L. https://books.google.com/books?id=XHEKAAAAIAAJ&pg=PA163. 
  4. ↑ Sharp, N.A.. "M22, NGC 6656". NOIRLab. https://noirlab.edu/public/images/noao-m22/. 
  5. ↑ O'Meara, Stephen James (2012). Deep-Sky Companions: Southern gems. Cambridge: Cambridge University Press. pp. 243–245. ISBN 978-1-107-01501-2. https://books.google.com/books?id=S5QIEKns33sC&pg=PA244. Retrieved September 24, 2021. 
  6. ↑ "Omega Centauri" (in en). European Southern Observatory. https://www.eso.org/public/france/images/b09/?lang. 
  7. ↑ 7.0 7.1 Messier, Charles (1771). "Catalogue des Nébuleuses & des amas d'Étoiles, que l'on découvre parmi les Étoiles fixes sur l'horizon de Paris; observées à l'Observatoire de la Marine, avec differens instruments" (in fr). Histoire de l'Académie Royale des Sciences ... Avec les Mémoires de Mathématique & de Physique, pour la même Année, ... [History of the Royal Academy of Sciences ... with the Mathematical and Physical Memoirs, for the same year, ...]: 435–461. https://gallica.bnf.fr/ark:/12148/bpt6k35697/f613.image. 
  8. ↑ Boyd, Richard N. (2008). An Introduction to Nuclear Astrophysics. University of Chicago Press. p. 376. ISBN 978-0-226-06971-5. https://books.google.com/books?id=uoIyc538X9kC. 
  9. ↑ Cite error: Invalid <ref> tag; no text was provided for refs named Moore-2003
  10. ↑ 10.0 10.1 Cudnik, Brian (2012). Faint Objects and How to Observe Them. Springer Science & Business Media. p. 8. ISBN 978-1-4419-6756-5. https://books.google.com/books?id=ZsY5NuwjdTEC&pg=PA8. 
  11. ↑ 11.0 11.1 Chen, James L. (2015). A Guide to Hubble Space Telescope Objects: Their selection, location, and significance. Illustrated by Adam Chen. Springer. p. 110. ISBN 978-3-319-18872-0. https://books.google.com/books?id=qj0wCgAAQBAJ&pg=PA110. 
  12. ↑ 12.0 12.1 Herschel, William (1789). "Catalogue of a second thousand of new nebulæ and clusters of stars, with a few introductory remarks on the construction of the heavens". Philosophical Transactions of the Royal Society of London 79: 212–255. Bibcode: 1789RSPT...79..212H. https://babel.hathitrust.org/cgi/pt?id=pst.000008680679;view=1up;seq=248. Retrieved April 28, 2021. 
  13. ↑ 13.0 13.1 Frommert, Hartmut; Kronberg, Christine. "Globular Star Clusters". Students for the Exploration and Development of Space. http://messier.seds.org/glob.html. 
  14. ↑ 14.0 14.1 Ashman, Keith M.; Zepf, Stephen E. (1998). Globular Cluster Systems. Cambridge Astrophysics Series. 30. Cambridge, UK University Press. p. 2. ISBN 978-0-521-55057-4. https://books.google.com/books?id=sXwXfSH6g90C. 
  15. ↑ Shapley, Harlow (1918). "Globular clusters and the structure of the galactic system". Publications of the Astronomical Society of the Pacific 30 (173): 42–54. doi:10.1086/122686. Bibcode: 1918PASP...30...42S. 
  16. ↑ Trimble, V.L. (December 1995). "The 1920 Shapley-Curtis Discussion: Background, issues, and aftermath". Publications of the Astronomical Society of the Pacific 107: 1133. doi:10.1086/133671. Bibcode: 1995PASP..107.1133T. https://escholarship.org/uc/item/1q68k7m0. 
  17. ↑ Bennett, Jeffrey O.; Donahue, Megan; Schneider, Nicholas; Voit, Mark (2020). The Cosmic Perspective (9th ed.). Pearson. ISBN 978-0-134-87436-4. 
  18. ↑ Zeilik, Michael; Gregory, Stephen A (1998). Introductory Astronomy & Astrophysics (4th ed.). Belmont Drive, CA: Brooks/Cole, Cengage Learning. p. 277. ISBN 978-0-03-006228-5. 
  19. ↑ Ryden, Barbara Sue; Peterson, Bradley M. (2010). Foundations of Astrophysics. San Francisco, CA. p. 436. ISBN 978-0-321-59558-4. 
  20. ↑ "Hubble images a swarm of ancient stars". European Space Agency (ESA). https://esahubble.org/images/opo9926a/. 
  21. ↑ Frommert, Hartmut (August 2007). "Milky Way Globular Clusters". Students for the Exploration and Development of Space. http://spider.seds.org/spider/MWGC/mwgc.html. 
  22. ↑ Carroll, Bradley W. (2017). An introduction to modern astrophysics (2nd ed.). Cambridge, United Kingdom: Cambridge University Press. p. 894. ISBN 978-1-108-42216-1. https://books.google.com/books?id=PY0wDwAAQBAJ&pg=PA894. Retrieved September 24, 2021. 
  23. ↑ Camargo, D.; Minniti, D. (2019). "Three candidate globular clusters discovered in the Galactic bulge". Monthly Notices of the Royal Astronomical Society: Letters 484: L90–L94. doi:10.1093/mnrasl/slz010. 
  24. ↑ Ashman, Keith M.; Zepf, Stephen E. (1992). "The formation of globular clusters in merging and interacting galaxies, Part 1". Astrophysical Journal 384: 50–61. doi:10.1086/170850. Bibcode: 1992ApJ...384...50A. 
  25. ↑ Barmby, P.; Huchra, J.P. (2001). "M31 globular clusters in the Hubble Space Telescope Archive. I. Cluster detection and completeleness". The Astronomical Journal 122 (5): 2458–2468. doi:10.1086/323457. Bibcode: 2001AJ....122.2458B. 
  26. ↑ Harris, William E. (1991). "Globular cluster systems in galaxies beyond the Local Group". Annual Review of Astronomy and Astrophysics 29 (1): 543–579. doi:10.1146/annurev.aa.29.090191.002551. Bibcode: 1991ARA&A..29..543H. 
  27. ↑ McLaughlin, Dean E.; Harris, William E.; Hanes, David A. (1994). "The spatial structure of the M87 globular cluster system". Astrophysical Journal 422 (2): 486–507. doi:10.1086/173744. Bibcode: 1994ApJ...422..486M. 
  28. ↑ Hogg, Helen Battles Sawyer (1965). "Harlow Shapley and globular glusters". Publications of the Astronomical Society of the Pacific 77 (458): 336–346. doi:10.1086/128229. Bibcode: 1965PASP...77..336S. 
  29. ↑ "The Very Large Telescope discovers new kind of globular star cluster". Astronomy. May 13, 2015. http://www.astronomy.com/news/2015/05/the-very-large-telescope-discovers-new-kind-of-globular-star-cluster. 
  30. ↑ Piotto, G.; Bedin, L. R.; Anderson, J.; King, I. R.; Cassisi, S.; Milone, A.P.; Villanova, S.; Pietrinferni, A. et al. (May 2007). "A Triple Main Sequence in the Globular Cluster NGC 2808". The Astrophysical Journal 661 (1): L53–L56. doi:10.1086/518503. Bibcode: 2007ApJ...661L..53P. 
  31. ↑ 31.0 31.1 31.2 Gratton, Raffaele; Bragaglia, Angela; Carretta, Eugenio; D'Orazi, Valentina; Lucatello, Sara; Sollima, Antonio (2019). "What is a globular cluster? An observational perspective". The Astronomy and Astrophysics Review 27 (1): 8. doi:10.1007/s00159-019-0119-3. Bibcode: 2019A&ARv..27....8G. 
  32. ↑ 32.0 32.1 Bastian, Nate; Lardo, Carmela (September 14, 2018). "Multiple Stellar Populations in Globular Clusters". Annual Review of Astronomy and Astrophysics 56 (1): 83–136. doi:10.1146/annurev-astro-081817-051839. Bibcode: 2018ARA&A..56...83B. 
  33. ↑ Piotto, Giampaolo (June 2009). "Observations of multiple populations in star clusters". 258. pp. 233–244. doi:10.1017/S1743921309031883. Bibcode: 2009IAUS..258..233P. 
  34. ↑ Weaver, D.; Villard, R.; Christensen, L. L.; Piotto, G.; Bedin, L. (May 2, 2007). "Hubble Finds Multiple Stellar 'Baby Booms' in a Globular Cluster". Hubble News Desk. http://hubblesite.org/newscenter/archive/releases/2007/18/full/. 
  35. ↑ Amaro-Seoane, P.; Konstantinidis, S.; Brem, P.; Catelan, M. (2013). "Mergers of multimetallic globular clusters: the role of dynamics". Monthly Notices of the Royal Astronomical Society 435 (1): 809–821. doi:10.1093/mnras/stt1351. Bibcode: 2013MNRAS.435..809A. 
  36. ↑ Mucciarelli, Alessio; Christensen, Lars Lindberg (September 10, 2014). "This Star Cluster Is Not What It Seems" (Press release). European Southern Observatory. eso1428. Retrieved April 7, 2021.
  37. ↑ Elmegreen, B. G.; Efremov, Y. N. (1999). "A Universal Formation Mechanism for Open and Globular Clusters in Turbulent Gas". Astrophysical Journal 480 (2): 235–245. doi:10.1086/303966. Bibcode: 1997ApJ...480..235E. 
  38. ↑ Lotz, Jennifer M.; Miller, Bryan W.; Ferguson, Henry C. (September 2004). "The Colors of Dwarf Elliptical Galaxy Globular Cluster Systems, Nuclei, and Stellar Halos". The Astrophysical Journal 613 (1): 262–278. doi:10.1086/422871. Bibcode: 2004ApJ...613..262L. 
  39. ↑ Burkert, Andreas; Tremaine, Scott (April 1, 2010). "A correlation between central supermassive black holes and the globular cluster systems of early-type galaxies". The Astrophysical Journal 720 (1): 516–521. doi:10.1088/0004-637X/720/1/516. Bibcode: 2010ApJ...720..516B. "A possible explanation is that both large black-hole masses and large globular cluster populations are associated with recent major mergers.". 
  40. ↑ Negueruela, Ignacio; Clark, Simon (March 22, 2005). "Young and Exotic Stellar Zoo: ESO's Telescopes Uncover Super Star Cluster in the Milky Way" (Press release). European Southern Observatory. eso0510. Archived from the original on April 9, 2007. Retrieved April 7, 2021.
  41. ↑ Kravtsov, V. V. (2001). "Globular Clusters and Dwarf Spheroidal Galaxies of the Outer Galactic Halo: on the Putative Scenario of their Formation". Astronomical and Astrophysical Transactions 20 (1): 89–92. doi:10.1080/10556790108208191. Bibcode: 2001A&AT...20...89K. 
  42. ↑ Bekki, K.; Freeman, K. C. (2003). "Formation of ω Centauri from an ancient nucleated dwarf galaxy in the young Galactic disc: Formation of ω Centauri". Monthly Notices of the Royal Astronomical Society 346 (2): L11–L15. doi:10.1046/j.1365-2966.2003.07275.x. Bibcode: 2003MNRAS.346L..11B. 
  43. ↑ Johnson, Christian I.; Dupree, Andrea K.; Mateo, Mario; Bailey, John I.; Olszewski, Edward W.; Walker, Matthew G. (2020). "The Most Metal-poor Stars in Omega Centauri (NGC 5139)". The Astronomical Journal 159 (6): 254. doi:10.3847/1538-3881/ab8819. Bibcode: 2020AJ....159..254J. 
  44. ↑ "Engulfed by Stars Near the Milky Way's Heart". European Space Agency (ESA). http://www.spacetelescope.org/images/potw1126a/. 
  45. ↑ Bastian, N.; Strader, J. (October 1, 2014). "Constraining globular cluster formation through studies of young massive clusters – III. A lack of gas and dust in massive stellar clusters in the LMC and SMC". Monthly Notices of the Royal Astronomical Society 443 (4): 3594–3600. doi:10.1093/mnras/stu1407. 
  46. ↑ Talpur, Jon (1997). "A Guide to Globular Clusters". Keele University. http://www.astro.keele.ac.uk/workx/globulars/globulars.html. 
  47. ↑ Mamajek, Eric. "Number Densities of Stars of Different Types in the Solar Vicinity". University of Rochester. http://www.pas.rochester.edu/~emamajek/memo_star_dens.html. 
  48. ↑ Smail, Ian. "The Hertzsprung-Russell Diagram of a Globular Cluster". University of Durham. http://www.dur.ac.uk/ian.smail/gcCm/gcCm_intro.html. 
  49. ↑ "Colorful Stars Galore Inside Globular Star Cluster Omega Centauri". NASA. September 9, 2009. https://www.nasa.gov/mission_pages/hubble/multimedia/ero/ero_omega_centauri.html. 
  50. ↑ Sigurdsson, Steinn (1992). "Planets in globular clusters?". Astrophysical Journal 399 (1): L95–L97. doi:10.1086/186615. Bibcode: 1992ApJ...399L..95S. 
  51. ↑ Arzoumanian, Z.; Joshi, K.; Rasio, F. A.; Thorsett, S.E. (1999). "Orbital Parameters of the PSR B1620-26 Triple System". Proceedings of the 160th Colloquium of the International Astronomical Union 105: 525. Bibcode: 1996ASPC..105..525A. 
  52. ↑ Bekki, K.; Freeman, K.C. (December 2003). "Formation of ω Centauri from an ancient nucleated dwarf galaxy in the young Galactic disc". Monthly Notices of the Royal Astronomical Society 346 (2): L11–L15. doi:10.1046/j.1365-2966.2003.07275.x. Bibcode: 2003MNRAS.346L..11B. 
  53. ↑ Forbes, Duncan A.; Bridges, Terry (January 25, 2010). "Accreted versus in situ Milky Way globular clusters". Monthly Notices of the Royal Astronomical Society 404 (3): 1203. doi:10.1111/j.1365-2966.2010.16373.x. Bibcode: 2010MNRAS.404.1203F. 
  54. ↑ Forbes, Duncan A.; Bastian, Nate; Gieles, Mark; Crain, Robert A.; Kruijssen, J. M. Diederik; Larsen, Søren S.; Ploeckinger, Sylvia; Agertz, Oscar et al. (February 2018). "Globular cluster formation and evolution in the context of cosmological galaxy assembly: open questions". Proceedings of the Royal Society A: Mathematical, Physical and Engineering Sciences 474 (2210): 20170616. doi:10.1098/rspa.2017.0616. PMID 29507511. Bibcode: 2018RSPSA.47470616F. 
  55. ↑ Green, Simon F.; Jones, Mark H.; Burnell, S. Jocelyn (2004). An Introduction to the Sun and Stars. Cambridge University Press. p. 240. ISBN 978-0-521-54622-5. 
  56. ↑ 56.0 56.1 van Albada, T. S.; Baker, Norman (1973). "On the Two Oosterhoff Groups of Globular Clusters". Astrophysical Journal 185: 477–498. doi:10.1086/152434. Bibcode: 1973ApJ...185..477V. 
  57. ↑ Buonanno, R.; Corsi, C.E.; Pulone, L. (1995). "ESO 280-SC06". Astronomical Journal 109: 663. doi:10.1086/117309. Bibcode: 1995AJ....109..663B. 
  58. ↑ Frommert, Hartmut. "Globular cluster ESO 280-S C06, in Ara". http://spider.seds.org/spider/MWGC/eso280sc06.html. 
  59. ↑ Harris, W.E. (1976). "Spatial structure of the globular cluster system and the distance to the galactic center". Astronomical Journal 81: 1095–1116. doi:10.1086/111991. Bibcode: 1976AJ.....81.1095H. 
  60. ↑ Lee, Y.W.; Yoon, S.J. (2002). "On the Construction of the Heavens". An Aligned Stream of Low-Metallicity Clusters in the Halo of the Milky Way 297 (5581): 578–581. doi:10.1126/science.1073090. PMID 12142530. Bibcode: 2002Sci...297..578Y. 
  61. ↑ "Spot the Difference – Hubble spies another globular cluster, but with a secret". Picture of the Week. ESA/Hubble. http://spacetelescope.org/images/potw1140a/. 
  62. ↑ "APOD: 2021 February 7 – Blue Straggler Stars in Globular Cluster M53". https://apod.nasa.gov/apod/ap210207.html. 
  63. ↑ 63.0 63.1 Baumgardt, Holger; Hut, Piet; Makino, Junichiro; McMillan, Steve; Portegies Zwart, Simon (2003). "On the Central Structure of M15". Astrophysical Journal Letters 582 (1): 21. doi:10.1086/367537. Bibcode: 2003ApJ...582L..21B. 
  64. ↑ 64.0 64.1 Vitral, E. (2023). "An elusive dark central mass in the globular cluster M4". Monthly Notices of the Royal Astronomical Society 522 (4): 5740–5757. doi:10.1093/mnras/stad1068. Bibcode: 2023MNRAS.522.5740V. 
  65. ↑ 65.0 65.1 "NASA's Hubble Hunts for Intermediate-Sized Black Hole Close to Home". NASA. 23 May 2023. https://www.nasa.gov/feature/goddard/2023/nasas-hubble-hunts-for-intermediate-sized-black-hole-close-to-home/. 
  66. ↑ Savage, D.; Neal, N.; Villard, R.; Johnson, R.; Lebo, H. (September 17, 2002). "Hubble discovers black holes in unexpected places". Space Telescope Science Institute. http://hubblesite.org/newscenter/newsdesk/archive/releases/2002/18/text/. 
  67. ↑ Finley, Dave (May 28, 2007). "Star cluster holds midweight black hole, VLA indicates". NRAO. http://www.nrao.edu/pr/2007/globularbh/. 
  68. ↑ 68.0 68.1 Greene, Jenny E.; Strader, Jay; Ho, Luis C. (August 18, 2020). "Intermediate-Mass Black Holes". Annual Review of Astronomy and Astrophysics 58 (1): 257–312. doi:10.1146/annurev-astro-032620-021835. Bibcode: 2020ARA&A..58..257G. 
  69. ↑ Baumgardt, Holger; Hut, Piet; Makino, Junichiro; McMillan, Steve; Portegies Zwart, Simon (2003). "A dynamical model for the globular cluster G1". Astrophysical Journal Letters 589 (1): 25. doi:10.1086/375802. Bibcode: 2003ApJ...589L..25B. 
  70. ↑ Tremou, Evangelia; Strader, Jay; Chomiuk, Laura; Shishkovsky, Laura; Maccarone, Thomas J.; Miller-Jones, James C. A.; Tudor, Vlad; Heinke, Craig O. et al. (July 18, 2018). "The MAVERIC Survey: Still No Evidence for Accreting Intermediate-mass Black Holes in Globular Clusters". The Astrophysical Journal 862 (1): 16. doi:10.3847/1538-4357/aac9b9. Bibcode: 2018ApJ...862...16T. 
  71. ↑ Baumgardt, H.; He, C.; Sweet, S. M.; Drinkwater, M.; Sollima, A.; Hurley, J.; Usher, C.; Kamann, S. et al. (2019). "No evidence for intermediate-mass black holes in the globular clusters ω Cen and NGC 6624". Monthly Notices of the Royal Astronomical Society 488 (4): 5340. doi:10.1093/mnras/stz2060. Bibcode: 2019MNRAS.488.5340B. 
  72. ↑ Woodrow, Janice (1991). "The Hertzsprung-Russell Diagram: Explaining a difficult concept". The Science Teacher 58 (8): 52–57. ISSN 0036-8555. 
  73. ↑ 73.0 73.1 73.2 Carroll, Bradley W.; Ostlie, Dale A. (2017). An Introduction to Modern Astrophysics (Second ed.). Cambridge, United Kingdom. pp. 475–476. ISBN 978-1-108-42216-1. 
  74. ↑ Schwarzschild, Martin (1958). Structure and Evolution of Stars. Princeton University Press. ISBN 978-0-486-61479-3. https://archive.org/details/StructureAndEvolutionOfTheStars. 
  75. ↑ "Observational Approach to Evolution. III. Semiempirical Evolution Tracks for M67 and M3". Astrophysical Journal 126: 326. 1957. doi:10.1086/146405. Bibcode: 1957ApJ...126..326S. 
  76. ↑ Piotto, G.; Milone, A. P.; Bedin, L. R.; Anderson, J.; King, I. R.; Marino, A. F.; Nardiello, D.; Aparicio, A. et al. (February 5, 2015). "The Hubble Space Telescope UV Legacy Survey of Galactic Globular Clusters. I. Overview of the Project and Detection of Multiple Stellar Populations". The Astronomical Journal 149 (3): 91. doi:10.1088/0004-6256/149/3/91. Bibcode: 2015AJ....149...91P. 
  77. ↑ Kalirai, J. S.; Richer, H. B. (2010). "Star clusters as laboratories for stellar and dynamical evolution". Philosophical Transactions of the Royal Society of London, Series A 368 (1913): 755–82. doi:10.1098/rsta.2009.0257. PMID 20083505. Bibcode: 2010RSPTA.368..755K. "Verification of the picture above came from extremely precise HST/ACS imaging observations of NGC 2808 by Piotto et al. (2007), who resolve three main sequences in the cluster for a single turnoff (see figure 3). This remarkable observation is consistent with multiple stellar populations of approximately the same age with varying helium abundances". 
  78. ↑ Majaess, D.; Turner, D.; Gieren, W.; Lane, D. (2012). "The Impact of Contaminated RR Lyrae/Globular Cluster Photometry on the Distance Scale". The Astrophysical Journal 752 (1): L10. doi:10.1088/2041-8205/752/1/L10. Bibcode: 2012ApJ...752L..10M. 
  79. ↑ Lee, Jae-Woo; López-Morales, Mercedes; Hong, Kyeongsoo; Kang, Young-Woon; Pohl, Brian L.; Walker, Alistair (2014). "Toward a Better Understanding of the Distance Scale from RR Lyrae Variable Stars: A Case Study for the Inner Halo Globular Cluster NGC 6723". The Astrophysical Journal Supplement Series 210 (1): 6. doi:10.1088/0067-0049/210/1/6. Bibcode: 2014ApJS..210....6L. 
  80. ↑ Cite error: Invalid <ref> tag; no text was provided for refs named :0
  81. ↑ Hansen, B. M. S.; Brewer, J.; Fahlman, G. G.; Gibson, B. K.; Ibata, R.; Limongi, M.; Rich, R. M.; Richer, H. B. et al. (2002). "The White Dwarf Cooling Sequence of the Globular Cluster Messier 4". Astrophysical Journal Letters 574 (2): L155. doi:10.1086/342528. Bibcode: 2002ApJ...574L.155H. 
  82. ↑ Soderblom, David R. (August 2010). "The Ages of Stars". Annual Review of Astronomy and Astrophysics 48 (1): 581–629. doi:10.1146/annurev-astro-081309-130806. Bibcode: 2010ARA&A..48..581S. 
  83. ↑ Chaboyer, Brian (1995). "Absolute ages of globular clusters and the age of the universe". The Astrophysical Journal 444: L9. doi:10.1086/187847. Bibcode: 1995ApJ...444L...9C. 
  84. ↑ Valcin, David; Bernal, José Luis; Jimenez, Raul; Verde, Licia; Wandelt, Benjamin D. (2020). "Inferring the age of the universe with globular clusters". Journal of Cosmology and Astroparticle Physics 2020 (12): 002. doi:10.1088/1475-7516/2020/12/002. Bibcode: 2020JCAP...12..002V. 
  85. ↑ Majaess, D. (February 23, 2013). "Nearby Ancient Star is Almost as Old as the Universe". Universe Today. http://www.universetoday.com/100147/nearby-ancient-star-is-almost-as-old-as-the-universe/. 
  86. ↑ "Ashes from the Elder Brethren" (Press release). European Southern Observatory. March 2, 2001. eso0107. Retrieved April 7, 2021.
  87. ↑ Staneva, A.; Spassova, N.; Golev, V. (1996). "The Ellipticities of Globular Clusters in the Andromeda Galaxy". Astronomy and Astrophysics Supplement 116 (3): 447–461. doi:10.1051/aas:1996127. Bibcode: 1996A&AS..116..447S. 
  88. ↑ Hensley, Kerrin (June 20, 2018). "Dating the Evaporation of Globular Clusters". https://astrobites.org/2018/06/20/dating-globular-clusters/. 
  89. ↑ Bose, Sownak; Ginsburg, Idan; Loeb, Abraham (May 23, 2018). "Dating the Tidal Disruption of Globular Clusters with GAIA Data on Their Stellar Streams". The Astrophysical Journal 859 (1): L13. doi:10.3847/2041-8213/aac48c. Bibcode: 2018ApJ...859L..13B. 
  90. ↑ 90.0 90.1 90.2 90.3 Benacquista, Matthew J. (2006). "Globular cluster structure". Living Reviews in Relativity 9 (1): 2. doi:10.12942/lrr-2006-2. PMID 28163652. Bibcode: 2006LRR.....9....2B. 
  91. ↑ Baumgardt, H; Hilker, M (August 1, 2018). "A catalogue of masses, structural parameters, and velocity dispersion profiles of 112 Milky Way globular clusters". Monthly Notices of the Royal Astronomical Society 478 (2): 1520–1557. doi:10.1093/mnras/sty1057. Bibcode: 2018MNRAS.478.1520B. 
  92. ↑ Zocchi, A.; Varri, A. L.; Bertin, Giuseppe (January 6, 2012). "A dynamical study of Galactic globular clusters under different relaxation conditions". Astronomy & Astrophysics 539: A65. doi:10.1051/0004-6361/201117977. Bibcode: 2012A&A...539A..65Z. https://www.researchgate.net/publication/51978934. 
  93. ↑ Frenk, C. S.; White, S. D. M. (1980). "The ellipticities of Galactic and LMC globular clusters". Monthly Notices of the Royal Astronomical Society 286 (3): L39–L42. doi:10.1093/mnras/286.3.l39. Bibcode: 1997MNRAS.286L..39G. 
  94. ↑ "Appearances can be deceptive". ESO Picture of the Week. potw1303a. http://www.spacetelescope.org/images/potw1303a/. 
  95. ↑ Kenneth Janes (November 2000). "Star Clusters". Encyclopedia of Astronomy and Astrophysics. p. 2. http://www.astro.caltech.edu/~george/ay20/eaa-starclus.pdf. 
  96. ↑ Rosen, Anna (July 18, 2012). "Understanding the Dynamical State of Globular Clusters". https://astrobites.org/2012/07/18/understanding-the-dynamical-state-of-globular-clusters/. 
  97. ↑ Chatterjee, Sourav; Umbreit, Stefan; Fregeau, John M.; Rasio, Frederic A. (March 11, 2013). "Understanding the dynamical state of globular clusters: core-collapsed versus non-core-collapsed". Monthly Notices of the Royal Astronomical Society 429 (4): 2881–2893. doi:10.1093/mnras/sts464. Bibcode: 2013MNRAS.429.2881C. 
  98. ↑ Van den Bergh, Sidney (November 2007). "Globular Clusters and Dwarf Spheroidal Galaxies". Monthly Notices of the Royal Astronomical Society 385 (1): L20–L22. doi:10.1111/j.1745-3933.2008.00424.x. Bibcode: 2008MNRAS.385L..20V. 
  99. ↑ Buonanno, R.; Corsi, C. E.; Buzzoni, A.; Cacciari, C.; Ferraro, F. R.; Fusi Pecci, F. (1994). "The Stellar Population of the Globular Cluster M 3. I. Photographic Photometry of 10 000 Stars". Astronomy and Astrophysics 290: 69–103. Bibcode: 1994A&A...290...69B. 
  100. ↑ Piatti, Andrés E.; Webb, Jeremy J.; Carlberg, Raymond G. (2019). "Characteristic radii of the Milky Way globular clusters". Monthly Notices of the Royal Astronomical Society 489 (3): 4367–4377. doi:10.1093/mnras/stz2499. 
  101. ↑ Da Costa, G. S.; Freeman, K. C. (May 1976). "The structure and mass function of the globular cluster M3". Astrophysical Journal 206 (1): 128–137. doi:10.1086/154363. Bibcode: 1976ApJ...206..128D. 
  102. ↑ Brosche, P.; Odenkirchen, M.; Geffert, M. (March 1999). "Instantaneous and average tidal radii of globular clusters". New Astronomy 4 (2): 133–139. doi:10.1016/S1384-1076(99)00014-7. Bibcode: 1999NewA....4..133B. 
  103. ↑ Djorgovski, S.; King, I. R. (1986). "A preliminary survey of collapsed cores in globular clusters". Astrophysical Journal 305: L61–L65. doi:10.1086/184685. Bibcode: 1986ApJ...305L..61D. https://authors.library.caltech.edu/97564/. 
  104. ↑ Bianchini, P; Webb, J J; Sills, A; Vesperini, E (March 21, 2018). "Kinematic fingerprint of core-collapsed globular clusters". Monthly Notices of the Royal Astronomical Society: Letters 475 (1): L96–L100. doi:10.1093/mnrasl/sly013. Bibcode: 2018MNRAS.475L..96B. 
  105. ↑ Ashman, Keith M.; Zepf, Stephen E. (1998). Globular Cluster Systems. Cambridge astrophysics series. 30. Cambridge University Press. p. 29. ISBN 978-0-521-55057-4. 
  106. ↑ Binney, James; Merrifield, Michael (1998). Galactic astronomy. Princeton series in astrophysics. Princeton University Press. p. 371. ISBN 978-0-691-02565-0. 
  107. ↑ Spitzer, Lyman (1984). "Dynamics of Globular Clusters". Science 225 (4661): 465–472. doi:10.1126/science.225.4661.465. ISSN 0036-8075. PMID 17750830. Bibcode: 1984Sci...225..465S. 
  108. ↑ Vanbeveren, D. (2001). The Influence of Binaries on Stellar Population Studies. Astrophysics and space science library. 264. Springer. p. 397. ISBN 978-0-7923-7104-5. 
  109. ↑ Spitzer, L. Jr. (June 2–4, 1986). "Dynamical Evolution of Globular Clusters". 267. Princeton, USA: Springer-Verlag, Berlin Heidelberg New York. p. 3. doi:10.1007/BFb0116388. ISBN 978-3-540-17196-6. Bibcode: 1986LNP...267....3S. 
  110. ↑ 110.0 110.1 Gnedin, Oleg Y.; Lee, Hyung Mok; Ostriker, Jeremiah P. (September 1999). "Effects of Tidal Shocks on the Evolution of Globular Clusters". The Astrophysical Journal 522 (2): 935–949. doi:10.1086/307659. Bibcode: 1999ApJ...522..935G. 
  111. ↑ Pooley, David (April 2010). "Effects of Tidal Shocks on the Evolution of Globular Clusters". Proceedings of the National Academy of Sciences 107 (16): 7164–7167. doi:10.1073/pnas.0913903107. PMID 20404204. Bibcode: 2010PNAS..107.7164P. 
  112. ↑ Bahcall, John N.; Piran, Tsvi; Weinberg, Steven (2004). Dark Matter in the Universe (2nd ed.). World Scientific. p. 51. ISBN 978-981-238-841-4. 
  113. ↑ "The stars of the Large Magellanic Cloud" (in en). June 20, 2016. https://esahubble.org/images/potw1625a/. 
  114. ↑ "Stellar Sorting in Globular Cluster 47" (Press release). Hubble News Desk. October 4, 2006. 2006-33. Retrieved April 9, 2021.
  115. ↑ Secker, Jeff (1992). "A Statistical Investigation into the Shape of the Globular cluster Luminosity Distribution". Astronomical Journal 104 (4): 1472–1481. doi:10.1086/116332. Bibcode: 1992AJ....104.1472S. 
  116. ↑ Heggie, D. C.; Giersz, M.; Spurzem, R.; Takahashi, K. (1998). "Dynamical Simulations: Methods and Comparisons". in Johannes Andersen. Kluwer Academic Publishers. p. 591. Bibcode: 1998HiA....11..591H. 
  117. ↑ Di Cintio, Pierfrancesco; Pasquato, Mario; Simon-Petit, Alicia; Yoon, Suk-Jin (2022). "Introducing a new multi-particle collision method for the evolution of dense stellar systems". Astronomy & Astrophysics 659: A19. doi:10.1051/0004-6361/202140710. 
  118. ↑ Benacquista, Matthew J. (2006). "Relativistic Binaries in Globular Clusters". Living Reviews in Relativity 9 (1): 2. doi:10.12942/lrr-2006-2. PMID 28163652. PMC 5255526. Bibcode: 2006LRR.....9....2B. http://relativity.livingreviews.org/Articles/lrr-2006-2/. Retrieved May 28, 2006. 
  119. ↑ Hasani Zonoozi, Akram (March 2011). "Direct N-body simulations of globular clusters – I. Palomar 14". Monthly Notices of the Royal Astronomical Society 411 (3): 1989–2001. doi:10.1111/j.1365-2966.2010.17831.x. Bibcode: 2011MNRAS.411.1989Z. 
  120. ↑ Dynamics of Star Clusters (International Astronomical Union Symposia). Springer. 1985. ISBN 978-90-277-1963-8. 
  121. ↑ Zhou, Yuan; Zhong, Xie Guang (June 1990). "The core evolution of a globular cluster containing massive black holes". Astrophysics and Space Science 168 (2): 233–241. doi:10.1007/BF00636869. Bibcode: 1990Ap&SS.168..233Y. 
  122. ↑ Pooley, Dave. "Globular Cluster Dynamics: the importance of close binaries in a real N-body system". self-published. http://www.deadlyastroninja.com/research/node1.html. 
  123. ↑ Yuan, Haibo; Liu, Xiaowei; Xiang, Maosheng; Huang, Yang; Chen, Bingqiu; Wu, Yue; Hou, Yonghui; Zhang, Yong (2015). "Stellar Loci Ii. A Model-Free Estimate of the Binary Fraction for Field FGK Stars". The Astrophysical Journal 799 (2): 135. doi:10.1088/0004-637X/799/2/135. Bibcode: 2015ApJ...799..135Y. 
  124. ↑ Sun, Weijia; De Grijs, Richard; Deng, Licai; Albrow, Michael D. (2021). "Binary-driven stellar rotation evolution at the main-sequence turn-off in star clusters". Monthly Notices of the Royal Astronomical Society 502 (3): 4350–4358. doi:10.1093/mnras/stab347. Bibcode: 2021MNRAS.502.4350S. 
  125. ↑ Duchêne, Gaspard; Kraus, Adam (August 18, 2013). "Stellar Multiplicity". Annual Review of Astronomy and Astrophysics 51 (1): 269–310. doi:10.1146/annurev-astro-081710-102602. Bibcode: 2013ARA&A..51..269D. 
  126. ↑ Cite error: Invalid <ref> tag; no text was provided for refs named murphy
  127. ↑ Giesers, Benjamin; Kamann, Sebastian; Dreizler, Stefan; Husser, Tim-Oliver; Askar, Abbas; Göttgens, Fabian; Brinchmann, Jarle; Latour, Marilyn et al. (2019). "A stellar census in globular clusters with MUSE: Binaries in NGC 3201". Astronomy & Astrophysics 632: A3. doi:10.1051/0004-6361/201936203. Bibcode: 2019A&A...632A...3G. 
  128. ↑ "Globular Cluster M10". ESA/Hubble Picture of the Week. http://www.spacetelescope.org/images/potw1225a/. 
  129. ↑ Ortolani, S.; Bica, E.; Barbuy, B. (1995). "BH 176 and AM-2: globular or open clusters?". Astronomy and Astrophysics 300: 726. Bibcode: 1995A&A...300..726O. 
  130. ↑ 130.0 130.1 Huxor, A. P.; Tanvir, N. R.; Irwin, M. J.; R. Ibata (2005). "A new population of extended, luminous, star clusters in the halo of M31". Monthly Notices of the Royal Astronomical Society 360 (3): 993–1006. doi:10.1111/j.1365-2966.2005.09086.x. Bibcode: 2005MNRAS.360.1007H. 
  131. ↑ Huxor, A. P.; Mackey, A. D.; Ferguson, A. M. N.; Irwin, M. J.; Martin, N. F.; Tanvir, N. R.; Veljanoski, J.; McConnachie, A. et al. (August 11, 2014). "The outer halo globular cluster system of M31 – I. The final PAndAS catalogue". Monthly Notices of the Royal Astronomical Society 442 (3): 2165–2187. doi:10.1093/mnras/stu771. 
  132. ↑ Ostriker, Jeremiah P.; Spitzer, Lyman Jr.; Chevalier, Roger A. (September 1972). "On the Evolution of Globular Clusters". Astrophysical Journal 176: L51. doi:10.1086/181018. Bibcode: 1972ApJ...176L..51O. 
  133. ↑ Lauchner, A.; Wilhelm, R.; Beers, T. C.; Allende Prieto, C. (December 2003). "A Search for Kinematic Evidence of Tidal Tails in Globular Clusters". Bibcode: 2003AAS...20311226L. 
  134. ↑ Di Matteo, P.; Miocchi, P.; Capuzzo Dolcetta, R. (May 2004). "Formation and Evolution of Clumpy Tidal Tails in Globular Clusters". Bibcode: 2004DDA....35.0303D. https://www.researchgate.net/publication/1799679. 
  135. ↑ Staude, Jakob (June 3, 2002). "Sky Survey Unveils Star Cluster Shredded By The Milky Way". Image of the Week (Press release). Sloan Digital Sky Survey. Archived from the original on June 29, 2006. Retrieved April 9, 2021.
  136. ↑ Carballo-Bello, J. A.; Corral-Santana, J. M.; Martínez-Delgado, D.; Sollima, A.; Muñoz, R. R.; Côté, P.; Duffau, S.; Catelan, M. et al. (January 24, 2017). "The southern leading and trailing wraps of the Sagittarius tidal stream around the globular cluster Whiting 1". Monthly Notices of the Royal Astronomical Society: Letters 467 (1): L91–L94. doi:10.1093/mnrasl/slx006. Bibcode: 2017MNRAS.467L..91C. 
  137. ↑ Dinescu, D. I.; Majewski, S. R.; Girard, T. M.; Cudworth, K. M. (2000). "The Absolute Proper Motion of Palomar 12: A Case for Tidal Capture from the Sagittarius Dwarf Spheroidal Galaxy". The Astronomical Journal 120 (4): 1892–1905. doi:10.1086/301552. Bibcode: 2000AJ....120.1892D. 
  138. ↑ Sbordone, L.; Bonifacio, P.; Buonanno, R.; Marconi, G.; Monaco, L.; Zaggia, S. (April 2007). "The exotic chemical composition of the Sagittarius dwarf spheroidal galaxy". Astronomy & Astrophysics 465 (3): 815–824. doi:10.1051/0004-6361:20066385. Bibcode: 2007A&A...465..815S. 
  139. ↑ Gnedin, Oleg Y.; Ostriker, Jeremiah P. (January 1997). "Destruction of the Galactic Globular Cluster System". The Astrophysical Journal 474 (1): 223–255. doi:10.1086/303441. Bibcode: 1997ApJ...474..223G. 
  140. ↑ Ricard, Elise (15 January 2016). "Planet locations, a supernova, and a black hole". California Academy of Sciences. https://www.calacademy.org/explore-science/space-friday-planet-locations-a-supernova-and-a-black-hole. 
  141. ↑ Gonzalez, Guillermo; Brownlee, Donald; Ward, Peter (July 2001). "The galactic habitable zone: Galactic chemical evolution". Icarus 152 (1): 185–200. doi:10.1006/icar.2001.6617. Bibcode: 2001Icar..152..185G. 
  142. ↑ Sigurdsson, S.; Stairs, I.H.; Moody, K.; Arzoumanian, K.M.Z.; Thorsett, S.E. (2008). "Planets around pulsars in globular clusters". in Fischer, D.; Rasio, F.A.; Thorsett, S.E. et al.. Extreme Solar Systems. ASP Conference Series. 398. Astronomical Society of the Pacific. p. 119. Bibcode: 2008ASPC..398..119S. 
  143. ↑ Spurzem, R. et al. (May 2009). "Dynamics of planetary systems in star clusters". The Astrophysical Journal 697 (1): 458–482. doi:10.1088/0004-637X/697/1/458. Bibcode: 2009ApJ...697..458S. 

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