V391 Pegasi
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Pegasus |
| Right ascension | 22h 04m 12.104s[1] |
| Declination | +26° 25′ 07.82″[1] |
| Apparent magnitude (V) | +14.61[2] |
| Characteristics | |
| Evolutionary stage | subdwarf B |
| Spectral type | sdB[3] |
| Variable type | V361 Hydrae (sdBVr)[4] |
| Astrometry | |
| Proper motion (μ) | RA: -4.822[1] mas/yr Dec.: 3.797[1] mas/yr |
| Parallax (π) | 0.8073 ± 0.0536 mas[1] |
| Distance | 4,000 ± 300 ly (1,240 ± 80 pc) |
| Absolute magnitude (MV) | +3.88[3] |
| Details | |
| Mass | 0.47[3] M☉ |
| Radius | 0.23[3] R☉ |
| Luminosity | 34[3] L☉ |
| Surface gravity (log g) | 5.4±0.1[5] cgs |
| Temperature | 29300 ± 500[5] K |
| Age | >10[6][7] Gyr |
| Other designations | |
HS 2201+2610, 2MASS J22041211+2625078 | |
| Database references | |
| SIMBAD | data |
V391 Pegasi, also catalogued as HS 2201+2610, is a blue-white subdwarf star approximately 4,000 light-years away in the constellation of Pegasus. The star is classified as an "extreme horizontal branch star". It is small, with only half the mass and a bit less than one quarter the diameter of the Sun. It has luminosity 34 times that of the Sun. It could be quite old, perhaps in excess of 10 Gyr. It is a pulsating variable star of the V361 Hydrae type (or also called sdBVr type). It is believed that the star's mass when it was still on the main sequence was between 0.8 and 0.9 times that of the Sun.[7]
Formation
Subdwarf B stars such as V391 Pegasi are thought to be the result of the ejection of the hydrogen envelope of a red giant star at or just before the onset of helium fusion. The ejection left only a tiny amount of hydrogen on the surface—less than 1/1000 of the total stellar mass. The future for the star is to eventually cool down to make a low-mass white dwarf. Most stars retain more of their hydrogen after the first red giant phase, and eventually become asymptotic giant branch stars. The reason that some stars, like V391 Pegasi, lose so much mass is not well known.[3] At the tip of the red-giant branch, the red giant precursors of the subdwarf stars reach their maximum radius, on the order of 0.7 AU.[6] After this point, the hydrogen envelope is lost and helium fusion begins—this is known as the helium flash.
Hypthesized planetary system
In 2007, research using the variable star timing method indicated the presence of a gas giant planet orbiting V391 Pegasi.[6] This planet was designated V391 Pegasi b. This planet around an "extreme horizontal branch" star provided clues about what could happen to the planets in the Solar System when the Sun turns into a red giant within the next 5 billion years.[8]
However, subsequent research published in 2018,[3] taking the large amount of new photometric time-series data amassed since the publication of the original data into account, found evidence both for and against the exoplanet's existence. Although the planet's existence was not disproved, the case for its existence was now certainly weaker, and the authors stated that it "requires confirmation with an independent method."
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | >3.2±0.7 MJ | 1.7±0.1 | 1170±44 | 0.00 | — | — |
References
- ^ a b c d e Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
- ^ Zacharias, N.; Finch, C. T.; Girard, T. M.; Henden, A.; Bartlett, J. L.; Monet, D. G.; Zacharias, M. I. (2012). "VizieR Online Data Catalog: UCAC4 Catalogue (Zacharias+, 2012)". Vizier Online Data Catalog. Bibcode:2012yCat.1322....0Z.
- ^ a b c d e f g Silvotti, R.; Schuh, S.; Kim, S.L.; Lutz, R.; Reed, M.; Benatti, S.; Janulis, R.; Lanteri, L.; Østensen, R.; Marsh, T.R.; Dhillon, V.S. (March 2018), "The sdB pulsating star V391 Peg and its putative giant planet revisited after 13 years of time-series photometric data.", Astronomy & Astrophysics, 611: A85, arXiv:1711.10942, Bibcode:2018A&A...611A..85S, doi:10.1051/0004-6361/201731473
- ^ Samus, N. N.; Durlevich, O. V.; et al. (2009), "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)", VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S, 1: B/gcvs, Bibcode:2009yCat....102025S
- ^ a b R. Østensen; J.-E. Solheim; U. Heber; R. Silvotti; et al. (2001), "Detection of pulsations in three subdwarf B stars", Astronomy and Astrophysics, 368 (1): 175–182, Bibcode:2001A&A...368..175O, doi:10.1051/0004-6361:20000488
- ^ a b c Silvotti, R.; Schuh, S.; Janulis, R.; Solheim, J. -E.; Bernabei, S.; Østensen, R.; Oswalt, T. D.; Bruni, I.; Gualandi, R.; Bonanno, A.; Vauclair, G.; Reed, M.; Chen, C. -W.; Leibowitz, E.; Paparo, M.; Baran, A.; Charpinet, S.; Dolez, N.; Kawaler, S.; Kurtz, D.; Moskalik, P.; Riddle, R.; Zola, S. (2007), "A giant planet orbiting the 'extreme horizontal branch' star V391 Pegasi" (PDF), Nature, 449 (7159): 189–91, Bibcode:2007Natur.449..189S, doi:10.1038/nature06143, PMID 17851517
- ^ a b Silvotti, R.; Schuh, S.; Janulis, R.; Solheim, J. -E.; Bernabei, S.; Østensen, R.; Oswalt, T. D.; Bruni, I.; Gualandi, R.; Bonanno, A.; Vauclair, G.; Reed, M.; Chen, C. -W.; Leibowitz, E.; Paparo, M.; Baran, A.; Charpinet, S.; Dolez, N.; Kawaler, S.; Kurtz, D.; Moskalik, P.; Riddle, R.; Zola, S. (2007), "A giant planet orbiting the 'extreme horizontal branch' star V391 Pegasi (Supplementary Information)" (PDF), Nature
- ^ Fortney, Jonathan (12 September 2007), "The one that got away", Nature, 449 (7159): 147–148, doi:10.1038/449147a
Sources
- C. S. Jeffery (2005). "Pulsations in Subdwarf B Stars". Journal of Astrophysics and Astronomy. 26 (2–3): 261–271. Bibcode:2005JApA...26..261J. doi:10.1007/BF02702334.
External links
- "Notes for star V391 Peg". The Extrasolar Planets Encyclopaedia. Retrieved 2008-06-24.
