HD 149026
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| 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 mas/yr[2] Dec.: 52.682 mas/yr[2] |
| Parallax (π) | 13.1203±0.0162 mas[2] |
| 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 | |
| Ogma, BD+38°2787, HD 149026, HIP 80838, SAO 65349, TOI-2024, TIC 255930614, GSC 03063-01587[4] | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | 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
[edit]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
[edit]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
[edit]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
[edit]References
[edit]- ^ Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015.
- ^ a b c d e f Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
- ^ a b c d e f g 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. arXiv:astro-ph/0507009. Bibcode:2005ApJ...633..465S. doi:10.1086/449306. S2CID 119026159.
- ^ a b c "HD 149026". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2009-05-20.
- ^ a b c d e f Carter, Joshua A.; et al. (2009). "Near-Infrared Transit Photometry of the Exoplanet HD 149026b". The Astrophysical Journal. 696 (1): 241–253. arXiv:0902.1542. Bibcode:2009ApJ...696..241C. doi:10.1088/0004-637X/696/1/241. S2CID 58943600.
- ^ a b "IAU Catalog of Star Names". Retrieved 28 July 2016.
- ^ NameExoWorlds: An IAU Worldwide Contest to Name Exoplanets and their Host Stars. IAU.org. 9 July 2014
- ^ "NameExoWorlds The Process". Archived from the original on 2015-08-15. Retrieved 2015-09-05.
- ^ Final Results of NameExoWorlds Public Vote Released, International Astronomical Union, 15 December 2015.
- ^ "NameExoWorlds The Approved Names". Archived from the original on 2018-02-01. Retrieved 2016-01-01.
- ^ "IAU Working Group on Star Names (WGSN)". Retrieved 22 May 2016.
- ^ "Bulletin of the IAU Working Group on Star Names, No. 1" (PDF). Retrieved 28 July 2016.
- ^ 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. arXiv:0802.2359. Bibcode:2008ApJ...685.1210L. doi:10.1086/591122. S2CID 14108418.
- ^ Harrington, Joseph; Luszcz, Statia; et al. (June 2007). "The hottest planet". Nature. 447 (7145): 691–693. Bibcode:2007Natur.447..691H. doi:10.1038/nature05863.
- ^ a b 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. arXiv:1710.07642. Bibcode:2018AJ....155...83Z. doi:10.3847/1538-3881/aaa458. S2CID 54755276.
- ^ 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. arXiv:1312.2954. Bibcode:2014ApJ...785..126K. doi:10.1088/0004-637X/785/2/126. S2CID 42687848.
- ^ Bonomo, A. S.; Desidera, 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. arXiv:1704.00373. Bibcode:2017A&A...602A.107B. doi:10.1051/0004-6361/201629882.
External links
[edit]- "N2K Information For Star HD149026". San Francisco State University. N2K Consortium. Archived from the original on 2008-04-20. Retrieved 2008-06-22.
- Naeye, Robert (2005-07-07). "Amateur Detects New Transiting Exoplanet". Sky & Telescope. Retrieved 2008-06-22.
- Naeye, Robert (2005-07-08). "One Big Ball of Rock". Sky & Telescope. Archived from the original on 2008-04-07. Retrieved 2008-06-22.
