Astronomy:Superluminal motion

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Short description: Apparent faster-than-light motion of distant astronomical objects
Superluminal motion

In astronomy, superluminal motion is the apparently faster-than-light motion seen in some radio galaxies, BL Lac objects, quasars, blazars and recently also in some galactic sources called microquasars. Bursts of energy moving out along the relativistic jets emitted from these objects can have a proper motion that appears greater than the speed of light. All of these sources are thought to contain a black hole, responsible for the ejection of mass at high velocities. Light echoes can also produce apparent superluminal motion.[1]

Explanation

Superluminal motion occurs as a special case of a more general phenomenon arising from the difference between the apparent speed of distant objects moving across the sky and their actual speed as measured at the source.[2]

In tracking the movement of such objects across the sky, a naive calculation of their speed can be derived by a simple distance divided by time calculation. If the distance of the object from the Earth is known, the angular speed of the object can be measured, and the speed can be naively calculated via:

apparent speed = distance to object [math]\displaystyle{ \times }[/math] angular speed.

This calculation does not yield the actual speed of the object, as it fails to account for the fact that the speed of light is finite. When measuring the movement of distant objects across the sky, there is a large time delay between what has been observed and what has occurred, due to the large distance the light from the distant object has to travel to reach us. The error in the above naive calculation comes from the fact that when an object has a component of velocity directed towards the Earth, as the object moves closer to the Earth that time delay becomes smaller. This means that the apparent speed as calculated above is greater than the actual speed. Correspondingly, if the object is moving away from the Earth, the above calculation underestimates the actual speed.

This effect in itself does not generally lead to superluminal motion being observed. But when the actual speed of the object is close to the speed of light, the apparent speed can be observed as greater than the speed of light, as a result of the above effect. As the actual speed of the object approaches the speed of light, the effect is most pronounced as the component of the velocity towards the Earth increases. This means that in most cases, 'superluminal' objects are travelling almost directly towards the Earth. However it is not strictly necessary for this to be the case, and superluminal motion can still be observed in objects with appreciable velocities not directed towards the Earth.[3]

Superluminal motion is most often observed in two opposing jets emanating from the core of a star or black hole. In this case, one jet is moving away from and one towards the Earth. If Doppler shifts are observed in both sources, the velocity and the distance can be determined independently of other observations.

Some contrary evidence

As early as 1983, at the "superluminal workshop" held at Jodrell Bank Observatory, referring to the seven then-known superluminal jets,

Schilizzi ... presented maps of arc-second resolution [showing the large-scale outer jets] ... which ... have revealed outer double structure in all but one (3C 273) of the known superluminal sources. An embarrassment is that the average projected size [on the sky] of the outer structure is no smaller than that of the normal radio-source population.[4]

In other words, the jets are evidently not, on average, close to the Earth's line-of-sight. (Their apparent length would appear much shorter if they were.)

In 1993, Thomson et al. suggested that the (outer) jet of the quasar 3C 273 is nearly collinear to the Earth's line-of-sight. Superluminal motion of up to ~9.6c has been observed along the (inner) jet of this quasar.[5][6][7]

Superluminal motion of up to 6c has been observed in the inner parts of the jet of M87. To explain this in terms of the "narrow-angle" model, the jet must be no more than 19° from the Earth's line-of-sight.[8] But evidence suggests that the jet is in fact at about 43° to the Earth's line-of-sight.[9] The same group of scientists later revised that finding and argue in favour of a superluminal bulk movement in which the jet is embedded.[10]

Suggestions of turbulence and/or "wide cones" in the inner parts of the jets have been put forward to try to counter such problems, and there seems to be some evidence for this.[11]

Signal velocity

The model identifies a difference between the information carried by the wave at its signal velocity c, and the information about the wave front's apparent rate of change of position. If a light pulse is envisaged in a wave guide (glass tube) moving across an observer's field of view, the pulse can only move at c through the guide. If that pulse is also directed towards the observer, he will receive that wave information, at c. If the wave guide is moved in the same direction as the pulse, the information on its position, passed to the observer as lateral emissions from the pulse, changes. He may see the rate of change of position as apparently representing motion faster than c when calculated, like the edge of a shadow across a curved surface. This is a different signal, containing different information, to the pulse and does not break the second postulate of special relativity. c is strictly maintained in all local fields.

Derivation of the apparent velocity

A relativistic jet coming out of the center of an active galactic nucleus is moving along AB with a velocity v, and is observed from the point O. At time [math]\displaystyle{ t_1 }[/math] a light ray leaves the jet from point A and another ray leaves at time [math]\displaystyle{ t_2=t_1+\delta t }[/math] from point B. An observer at O receives the rays at time [math]\displaystyle{ t_1^\prime }[/math] and [math]\displaystyle{ t_2^\prime }[/math] respectively. The angle [math]\displaystyle{ \phi }[/math] is small enough that the two distances marked [math]\displaystyle{ D_L }[/math] can be considered equal.

Superluminal motion in AGN jets.png
[math]\displaystyle{ AB = v \, \delta t }[/math]
[math]\displaystyle{ AC = v \, \delta t \cos\theta }[/math]
[math]\displaystyle{ BC = v \, \delta t \sin\theta }[/math]
[math]\displaystyle{ t_2-t_1 = \delta t }[/math]
[math]\displaystyle{ t_1' = t_1 + \frac{D_L + v \, \delta t \cos\theta}{c} }[/math]
[math]\displaystyle{ t_2' = t_2 + \frac{D_L}{c} }[/math]
[math]\displaystyle{ \delta t' = t_2' - t_1' = t_2 - t_1 - \frac{v \, \delta t \cos\theta}{c} = \delta t - \frac{v \, \delta t \cos\theta}{c} = \delta t (1-\beta \cos\theta) }[/math], where [math]\displaystyle{ \beta=v/c }[/math]
[math]\displaystyle{ \delta t = \frac{\delta t'}{1-\beta\cos\theta} }[/math]
[math]\displaystyle{ BC = D_L\sin\phi \approx \phi D_L = v \, \delta t \sin\theta \Rightarrow \phi D_L = v\sin\theta\frac{\delta t'}{1-\beta\cos\theta} }[/math]

Apparent transverse velocity along [math]\displaystyle{ CB }[/math], [math]\displaystyle{ v_\text{T} = \frac{\phi D_L}{\delta t'}=\frac{v\sin\theta}{1-\beta\cos\theta} }[/math]

[math]\displaystyle{ \beta_\text{T} = \frac{v_\text{T}}{c} = \frac{\beta\sin\theta}{1-\beta\cos\theta}. }[/math]

The apparent transverse velocity is maximal for angle ([math]\displaystyle{ 0 \lt \beta \lt 1 }[/math] is used)

[math]\displaystyle{ \frac{\partial\beta_\text{T}}{\partial\theta} = \frac{\partial}{\partial\theta} \left[\frac{\beta\sin\theta}{1-\beta\cos\theta}\right] = \frac{\beta\cos\theta}{1-\beta\cos\theta} - \frac{(\beta\sin\theta)^2}{(1-\beta\cos\theta)^2} = 0 }[/math]
[math]\displaystyle{ \Rightarrow \beta\cos\theta(1-\beta\cos\theta)^2 = (1 - \beta\cos\theta) (\beta\sin\theta)^2 }[/math]
[math]\displaystyle{ \Rightarrow \beta\cos\theta (1-\beta\cos\theta) = (\beta\sin\theta)^2 \Rightarrow \beta\cos\theta - \beta^2\cos^2\theta = \beta^2\sin^2\theta \Rightarrow \cos\theta_\text{max} = \beta }[/math]
[math]\displaystyle{ \Rightarrow \sin\theta_\text{max} = \sqrt{1-\cos^2\theta_\text{max}} = \sqrt{1-\beta^2} = \frac{1}{\gamma}\, }[/math], where [math]\displaystyle{ \gamma=\frac{1}{\sqrt{1-\beta^2}} }[/math]
[math]\displaystyle{ \therefore \beta_\text{T}^\text{max} = \frac{\beta\sin\theta_\text{max}}{1-\beta\cos\theta_\text{max}} = \frac{\beta/\gamma}{1-\beta^2} = \beta\gamma }[/math]

If [math]\displaystyle{ \gamma \gg 1 }[/math] (i.e. when velocity of jet is close to the velocity of light) then [math]\displaystyle{ \beta_\text{T}^\text{max} \gt 1 }[/math] despite the fact that [math]\displaystyle{ \beta \lt 1 }[/math]. And of course [math]\displaystyle{ \beta_\text{T} \gt 1 }[/math] means that the apparent transverse velocity along [math]\displaystyle{ CB }[/math], the only velocity on the sky that can be measured, is larger than the velocity of light in vacuum, i.e. the motion is apparently superluminal.

History

The apparent superluminal motion in the faint nebula surrounding Nova Persei was first observed in 1901 by Charles Dillon Perrine.[12] “Mr. Perrine’s photograph of November 7th and 8th, 1901, secured with the Crossley Reflector, led to the remarkable discovery that the masses of nebulosity were apparently in motion, with a speed perhaps several hundred times as great as hitherto observed.”[13] “Using the 36-in. telescope (Crossley), he discovered the apparent superluminal motion of the expanding light bubble around Nova Persei (1901). Thought to be a nebula, the visual appearance was actually caused by light from the nova event reflected from the surrounding interstellar medium as the light moved outward from the star. Perrine studied this phenomenon using photographic, spectroscopic, and polarization techniques.”[14]

Superluminal motion was first observed in 1902 by Jacobus Kapteyn in the ejecta of the nova GK Persei, which had exploded in 1901.[15] His discovery was published in the German journal Astronomische Nachrichten, and received little attention from English-speaking astronomers until many decades later.[16][17]

In 1966, Martin Rees pointed out that "an object moving relativistically in suitable directions may appear to a distant observer to have a transverse velocity much greater than the velocity of light".[18] In 1969 and 1970 such sources were found as very distant astronomical radio sources, such as radio galaxies and quasars,[19][20][21] and were called superluminal sources. The discovery was the result of a new technique called Very Long Baseline Interferometry, which allowed astronomers to set limits to the angular size of components and to determine positions to better than milli-arcseconds, and in particular to determine the change in positions on the sky, called proper motions, in a timespan of typically years. The apparent velocity is obtained by multiplying the observed proper motion by the distance, which could be up to 6 times the speed of light.

In the introduction to a workshop on superluminal radio sources, Pearson and Zensus reported

The first indications of changes in the structure of some sources were obtained by an American-Australian team in a series of transpacific VLBI observations between 1968 and 1970 (Gubbay et al. 1969).[19] Following the early experiments, they had realised the potential of the NASA tracking antennas for VLBI measurements and set up an interferometer operating between California and Australia. The change in the source visibility that they measured for 3C 279, combined with changes in total flux density, indicated that a component first seen in 1969 had reached a diameter of about 1 milliarcsecond, implying expansion at an apparent velocity of at least twice the speed of light. Aware of Rees's model,[18] (Moffet et al. 1972)[22] concluded that their measurement presented evidence for relativistic expansion of this component. This interpretation, although by no means unique, was later confirmed, and in hindsight it seems fair to say that their experiment was the first interferometric measurement of superluminal expansion.[23]

In 1994, a galactic speed record was obtained with the discovery of a superluminal source in the Milky Way, the cosmic x-ray source GRS 1915+105. The expansion occurred on a much shorter timescale. Several separate blobs were seen to expand in pairs within weeks by typically 0.5 arcsec.[24] Because of the analogy with quasars, this source was called a microquasar.

See also

Notes

  1. ↑ Bond, H. E. (2003). "An energetic stellar outburst accompanied by circumstellar light echoes". Nature 422 (6930): 405–408. doi:10.1038/nature01508. PMID 12660776. Bibcode: 2003Natur.422..405B. 
  2. ↑ Recami, Erasmo (April 1986). "Considerations about the apparent superluminal expansions observed in astrophysics". Il Nuovo Cimento 93 (1): 9. doi:10.1007/BF02722327. Bibcode: 1986NCimB..93..119R. 
  3. ↑ Meyer, Eileen (June 2018). "Detection of an Optical/UV Jet/Counterjet and Multiple Spectral Components in M84". The Astrophysical Journal 680 (1): 9. doi:10.3847/1538-4357/aabf39. Bibcode: 2018ApJ...860....9M. 
  4. ↑ Porcas, Richard (1983). "Superluminal motions: Astronomers still puzzled". Nature 302 (5911): 753–754. doi:10.1038/302753a0. Bibcode: 1983Natur.302..753P. 
  5. ↑ Thomson, R. C.; MacKay, C. D.; Wright, A. E. (1993). "Internal structure and polarization of the optical jet of the quasar 3C273". Nature 365 (6442): 133. doi:10.1038/365133a0. Bibcode: 1993Natur.365..133T. ;
  6. ↑ Pearson, T. J.; Unwin, S. C.; Cohen, M. H.; Linfield, R. P.; Readhead, A. C. S.; Seielstad, G. A.; Simon, R. S.; Walker, R. C. (1981). "Superluminal expansion of quasar 3C273". Nature 290 (5805): 365. doi:10.1038/290365a0. Bibcode: 1981Natur.290..365P. ;
  7. ↑ Davis, R. J.; Unwin, S. C.; Muxlow, T. W. B. (1991). "Large-scale superluminal motion in the quasar 3C273". Nature 354 (6352): 374. doi:10.1038/354374a0. Bibcode: 1991Natur.354..374D. 
  8. ↑ Biretta, John A.; Junor, William; Livio, Mario (1999). "Formation of the radio jet in M87 at 100 Schwarzschild radii from the central black hole". Nature 401 (6756): 891. doi:10.1038/44780. Bibcode: 1999Natur.401..891J.  ; Biretta, J. A.; Sparks, W. B.; MacChetto, F. (1999). "Hubble Space TelescopeObservations of Superluminal Motion in the M87 Jet". The Astrophysical Journal 520 (2): 621. doi:10.1086/307499. Bibcode: 1999ApJ...520..621B. 
  9. ↑ Biretta, J. A.; Zhou, F.; Owen, F. N. (1995). "Detection of Proper Motions in the M87 Jet". The Astrophysical Journal 447: 582. doi:10.1086/175901. Bibcode: 1995ApJ...447..582B. 
  10. ↑ Biretta, J. A.; Sparks, W. B.; MacChetto, F. (1999). "Hubble Space TelescopeObservations of Superluminal Motion in the M87 Jet". The Astrophysical Journal 520 (2): 621. doi:10.1086/307499. Bibcode: 1999ApJ...520..621B. 
  11. ↑ Biretta, John A.; Junor, William; Livio, Mario (1999). "Formation of the radio jet in M87 at 100 Schwarzschild radii from the central black hole". Nature 401 (6756): 891. doi:10.1038/44780. Bibcode: 1999Natur.401..891J. 
  12. ↑ Perrine, Charles (Dec 1901). "Motion in the faint nebula surrounding Nova Persei". Astrophysical Journal 14: 359–362. doi:10.1086/140877. Bibcode: 1901ApJ....14..359P. 
  13. ↑ Campbell, William (1902). "The Lick Observatory and It's Problems". Overland Monthly XL (3): 326–327. 
  14. ↑ Teare S.W. (2014). "Charles Dillon Perrine". Biographical Encyclopedia of Astronomers. doi:10.1007/978-1-4419-9917-7_1074. 
  15. ↑ Bode, M. F.; O'Brien, T. J.; Simpson, M. (2004). "Echoes of an Explosive Past: Solving the Mystery of the First Superluminal Source". The Astrophysical Journal 600 (1): L63–L66. doi:10.1086/381529. Bibcode: 2004ApJ...600L..63B. 
  16. ↑ Kapteyn's paper
  17. ↑ Index of citations to Kapteyn's paper
  18. ↑ 18.0 18.1 Rees, M. J. (1966). "Appearance of Relativistically Expanding Radio Sources". Nature 211 (5048): 468–470. doi:10.1038/211468a0. Bibcode: 1966Natur.211..468R. 
  19. ↑ 19.0 19.1 Gubbay, J.S.; Legg, A.J.; Robertson, D.S.; Moffet, A.T.; Ekers, R.D.; Seidel, B. (1969). "Variations of Small Quasar Components at 2,300 MHz". Nature 224 (5224): 1094–1095. doi:10.1038/2241094b0. Bibcode: 1969Natur.224.1094G. 
  20. ↑ Cohen, M. H.; Cannon, W.; Purcell, G. H.; Shaffer, D. B.; Broderick, J. J.; Kellermann, K. I.; Jauncey, D. L. (1971). "The Small-Scale Structure of Radio Galaxies and Quasi-Stellar Sources at 3.8 Centimeters". The Astrophysical Journal 170: 207. doi:10.1086/151204. Bibcode: 1971ApJ...170..207C. 
  21. ↑ Whitney, AR; Shapiro, Irwin I.; Rogers, Alan E. E.; Robertson, Douglas S.; Knight, Curtis A.; Clark, Thomas A.; Goldstein, Richard M.; Marandino, Gerard E. et al. (1971). "Quasars Revisited: Rapid Time Variations Observed Via Very-Long-Baseline Interferometry". Science 173 (3993): 225–30. doi:10.1126/science.173.3993.225. PMID 17741416. Bibcode: 1971Sci...173..225W. 
  22. ↑ Moffet, A.T.; Gubbay, J.; Robertson, D.S.; Legg, A.J. (1972). Evans, D.S. ed. External Galaxies and Quasi-Stellar Objects : IAU Symposium 44, held in Uppsala, Sweden 10-14 August 1970. Dordrecht: Reidel. p. 228. ISBN 9027701997. 
  23. ↑ Pearson, Timothy J.; Zensus, J. Anton (1987). J. Anton Zensus. ed. Superluminal Radio Sources: proceedings of a workshop in honor of Professor Marshall H. Cohen, held at Big Bear Solar Observatory, California, October 28-30, 1986. Cambridge; New York: Cambridge University Press. 3. ISBN 9780521345606. Bibcode: 1987slrs.work....1P. 
  24. ↑ Mirabel, I.F.; Rodriguez, L.F. (1994). "A superluminal source in the Galaxy". Nature 371 (6492): 46–48. doi:10.1038/371046a0. Bibcode: 1994Natur.371...46M. 

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