V391 Pegasi

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V391 Pegasi
V391PegLightCurve.png
A light curve for V391 Pegasi, adapted from Silvotti et al. (2010) [1]
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Pegasus
Right ascension 22h 04m 12.1045s [2]
Declination +26° 25′ 07.819″ [2]
Apparent magnitude  (V)+14.61 [3]
Characteristics
Evolutionary stage subdwarf B
Spectral type sdB [4]
Variable type V361 Hydrae (sdBVr) [5]
Astrometry
Proper motion (μ)RA: −4.906(40)  mas/yr [2]
Dec.: −3.703(34)  mas/yr [2]
Parallax (π)0.7388 ± 0.0327  mas [2]
Distance 4,400 ± 200  ly
(1,350 ± 60  pc)
Absolute magnitude  (MV)+3.88 [4]
Details
Mass 0.47 [4]   M☉
Radius 0.23 [4]   R☉
Luminosity 34 [4]   L☉
Surface gravity (log g)5.4±0.1 [6]   cgs
Temperature 29,300±500 [6]   K
Age >10 [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 4,400 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 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]

Contents

In 2001, Roy Østensen et al. announced that the star, then called HS 2201+2610, is a variable star. [8] It was given its variable star designation, V391 Pegasi, in 2003. [9] It is a pulsating variable star of the V361 Hydrae type (or also called sdBVr type).

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. [4] 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. [7] After this point, the hydrogen envelope is lost and helium fusion begins—this is known as the helium flash.

Hypothesized planetary system

In 2007, research using the variable star timing method indicated the presence of a gas giant planet orbiting V391 Pegasi. [7] 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. [10]

However, subsequent research published in 2018, [4] 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."

The V391 Pegasi planetary system
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b (unconfirmed)>3.2±0.7 MJ 1.7±0.11170±440.00——

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References

  1. ↑ Silvotti, R.; Randall, S. K.; Dhillon, V. S.; Marsh, T. R.; Savoury, C. D.; Schuh, S.; Fontaine, G.; Brassard, P. (December 2010). "V391 Peg: Identification of the two main pulsation modes from ULTRACAM u'g'r' amplitudes". Astronomische Nachrichten. 331: 1034–1037. arXiv: 1005.2840 . Bibcode:2010AN....331.1034S. doi:10.1002/asna.201011451. S2CID   119117121 . Retrieved 14 February 2022.
  2. 1 2 3 4 5 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.
  3. ↑ 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 On-line Data Catalog. Bibcode:2012yCat.1322....0Z.
  4. 1 2 3 4 5 6 7 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, S2CID   119492634
  5. ↑ 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
  6. 1 2 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
  7. 1 2 3 4 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, S2CID   4342338
  8. ↑ Østensen, R.; Solheim, J. E.; Heber, U.; Silvotti, R.; Dreizler, S.; Edelmann, H. (March 2001). "Detection of pulsations in three subdwarf B stars" (PDF). Astronomy and Astrophysics. 368: 175–182. doi:10.1051/0004-6361:20000488 . Retrieved 26 December 2024.
  9. ↑ Kazarovets, E. V.; Kireeva, N. N.; Samus, N. N.; Durlevich, O. V. (May 2003). "The 77th Name-List of Variable Stars" (PDF). Information Bulletin on Variable Stars. 5422: 1–56. Retrieved 26 December 2024.
  10. ↑ Fortney, Jonathan (12 September 2007), "The one that got away", Nature, 449 (7159): 147–148, Bibcode:2007Natur.449..147F, doi: 10.1038/449147a , PMID   17851500, S2CID   38288758

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