Astronomy:HD 149026
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Hercules[1] |
| Right ascension | 16h 30m 29.61858s[2] |
| Declination | +38° 20′ 50.3090″[2] |
| Apparent magnitude (V) | 8.15[3] |
| Characteristics | |
| Spectral type | G0 IV[3] |
| Apparent magnitude (B) | 8.76[4] |
| B−V color index | 0.611 |
| Astrometry | |
| Radial velocity (Rv) | −17.93±0.13[2] km/s |
| Proper motion (μ) | RA: −77.963[2] mas/yr Dec.: 52.682[2] mas/yr |
| Parallax (π) | 13.1203 ± 0.0162[2] mas |
| Distance | 248.6 ± 0.3 ly (76.22 ± 0.09 pc) |
| Absolute magnitude (MV) | 3.65±0.12[5] |
| Details | |
| Mass | 1.345±0.020[5] M☉ |
| Radius | 1.541+0.046−0.042[5] R☉ |
| Luminosity | 3.03+0.20−0.18[5] L☉ |
| Surface gravity (log g) | 4.189+0.020−0.021[5] cgs |
| Temperature | 6,147±50[3] K |
| Metallicity [Fe/H] | 0.36±0.05[3] dex |
| Rotational velocity (v sin i) | 6.0±0.5[3] km/s |
| Age | 2.6+0.3−0.2[5] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
| Extrasolar Planets Encyclopaedia | data |
HD 149026, also named Ogma /ˈɒɡmə/,[6] is a yellow subgiant star approximately 249 light-years from the Sun in the constellation of Hercules. An exoplanet (designated HD 149026 b, later named Smertrios) orbits the star.
Nomenclature
HD 149026 is the star's identifier in the Henry Draper Catalog.[4] Following its discovery in 2005 the planet was designated HD 149026 b.
In July 2014 the International Astronomical Union (IAU) launched NameExoWorlds, a process for giving proper names to certain exoplanets and their host stars.[7] The process involved public nomination and voting for the new names.[8] In December 2015, the IAU announced the winning names were Ogma for this star and Smertrios for its planet.[9]
The winning names based on those submitted by the Club d'Astronomie de Toussaint of France; namely 'Ogmios' and 'Smertrios'. Ogmios was a Gallo-Roman deity and Smertrios was a Gallic deity of war. The IAU substituted the name of Ogma, a deity of eloquence, writing, and great physical strength in the Celtic mythologies of Ireland and Scotland, and who may be related to Ogmios, because 'Ogmios' is the name of an asteroid (189011 Ogmios).[10]
In 2016, the IAU organized a Working Group on Star Names (WGSN)[11] to catalog and standardize proper names for stars. In its first bulletin of July 2016,[12] the WGSN explicitly recognized the names of exoplanets and their host stars approved by the Executive Committee Working Group Public Naming of Planets and Planetary Satellites, including the names of stars adopted during the 2015 NameExoWorlds campaign. This star is now so entered in the IAU Catalog of Star Names.[6]
Properties
The star is thought to be much more massive, larger and brighter than the Sun. The higher mass means that despite its considerably younger age (2.0 Ga) it is already much more evolved than the Sun. The internal fusion of hydrogen in the core of the star is coming to an end, and it is beginning to evolve towards red gianthood. At a distance of 249 light-years,[2] the star is not visible to the unaided eye. However, it should be easily seen in binoculars or a small telescope.[3]
The star is over twice as enriched with chemical elements heavier than hydrogen and helium as the Sun. Because of this and the fact that the star is relatively bright, a group of astronomers in N2K Consortium began to study the star. The star's anomalous composition as measured may be surface pollution only, from the intake of heavy-element planetesimals.[13]
Planetary system
In 2005 an unusual extrasolar planet was discovered to be orbiting the star. Designated HD 149026 b, it was detected transiting the star allowing its diameter to be measured. It was found to be smaller than other transiting planets known at the time, meaning it is unusually dense for a closely orbiting giant planet.[3] In 2007, the temperature of the giant planet was calculated to be 2,300 K (2,030 °C; 3,680 °F), generating so much infrared heat that it glows. It was proposed that the planet absorbs nearly all the sunlight and radiates it into space as heat.[14] Subsequent studies have not confirmed this, with a 2018 study finding the planet to be highly reflective (with a Bond albedo of 0.53), along with a lower temperature.[15]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b (Smertrios) | 0.324±0.011 MJ | 0.04364±0.00022 | 2.87588874(59)[15] | 0.0028+0.019 −0.0024 |
84.50+0.60 −0.52° |
0.811+0.029 −0.027 RJ |
See also
References
- ↑ Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331. doi:10.1134/S1063773712050015. Bibcode: 2012AstL...38..331A.
- ↑ 2.0 2.1 2.2 2.3 2.4 2.5 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940 Gaia DR3 record for this source at VizieR.
- ↑ 3.0 3.1 3.2 3.3 3.4 3.5 3.6 Sato, Bun'ei et al. (2005). "The N2K Consortium. II. A Transiting Hot Saturn around HD 149026 with a Large Dense Core". The Astrophysical Journal 633 (1): 465–473. doi:10.1086/449306. Bibcode: 2005ApJ...633..465S.
- ↑ 4.0 4.1 4.2 "HD 149026". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+149026.
- ↑ 5.0 5.1 5.2 5.3 5.4 5.5 Carter, Joshua A. et al. (2009). "Near-Infrared Transit Photometry of the Exoplanet HD 149026b". The Astrophysical Journal 696 (1): 241–253. doi:10.1088/0004-637X/696/1/241. Bibcode: 2009ApJ...696..241C.
- ↑ 6.0 6.1 "IAU Catalog of Star Names". http://www.pas.rochester.edu/~emamajek/WGSN/IAU-CSN.txt.
- ↑ NameExoWorlds: An IAU Worldwide Contest to Name Exoplanets and their Host Stars . IAU.org. 9 July 2014
- ↑ "NameExoWorlds The Process". http://nameexoworlds.iau.org/process.
- ↑ Final Results of NameExoWorlds Public Vote Released , International Astronomical Union, 15 December 2015.
- ↑ "NameExoWorlds The Approved Names". http://nameexoworlds.iau.org/names.
- ↑ "IAU Working Group on Star Names (WGSN)". https://www.iau.org/science/scientific_bodies/working_groups/280/.
- ↑ "Bulletin of the IAU Working Group on Star Names, No. 1". http://www.pas.rochester.edu/~emamajek/WGSN/WGSN_bulletin1.pdf.
- ↑ S.-L. Li; D. N. C. Lin; X.-W. Liu (2008). "Extent of pollution in planet-bearing stars". The Astrophysical Journal 685 (2): 1210–1219. doi:10.1086/591122. Bibcode: 2008ApJ...685.1210L.
- ↑ Harrington, Joseph et al. (June 2007). "The hottest planet". Nature 447 (7145): 691–693. doi:10.1038/nature05863. PMID 17495928. Bibcode: 2007Natur.447..691H.
- ↑ 15.0 15.1 Zhang, Michael et al. (2018). "Phase Curves of WASP-33b and HD 149026b and a New Correlation between Phase Curve Offset and Irradiation Temperature". The Astronomical Journal 155 (2): 83. doi:10.3847/1538-3881/aaa458. Bibcode: 2018AJ....155...83Z.
- ↑ Knutson, Heather A. et al. (2014). "Friends of Hot Jupiters. I. A Radial Velocity Search for Massive, Long-Period Companions to Close-In Gas Giant Planets". The Astrophysical Journal 785 (2): 126. doi:10.1088/0004-637X/785/2/126. Bibcode: 2014ApJ...785..126K.
- ↑ Bonomo, A. S. et al. (June 2017). "The GAPS Programme with HARPS-N at TNG. XIV. Investigating giant planet migration history via improved eccentricity and mass determination for 231 transiting planets". Astronomy & Astrophysics 602: A107. doi:10.1051/0004-6361/201629882. Bibcode: 2017A&A...602A.107B.
External links
- "N2K Information For Star HD149026". San Francisco State University. N2K Consortium. http://tauceti.sfsu.edu/n2k/hd149026/index.html.
- Naeye, Robert (2005-07-07). "Amateur Detects New Transiting Exoplanet". Sky & Telescope. http://www.skyandtelescope.com/news/3310446.html?page=1&c=y.
- Naeye, Robert (2005-07-08). "One Big Ball of Rock". Sky & Telescope. http://www.skyandtelescope.com/news/3310426.html?page=1&c=y.
Coordinates: 
16h 30m 29.619s, +38° 20′ 50.31″
 |  |
