Astronomy:Gliese 514

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Coordinates: Sky map 13h 29m 59.7859s, +10° 22′ 37.7845″

Gliese 514
Observation data
Equinox J2000.0]] (ICRS)
Constellation Virgo
Right ascension  13h 29m 59.7859s[1]
Declination 10° 22′ 37.7845″[1]
Apparent magnitude (V) 9.029
Characteristics
Evolutionary stage main-sequence star
Spectral type M0Ve[2]
Apparent magnitude (J) 5.902±0.018[3]
Apparent magnitude (H) 5.300±0.033[3]
Astrometry
Radial velocity (Rv)14.606[4] km/s
Proper motion (μ) RA: 1,127.34±0.03[5] mas/yr
Dec.: −1,073.888±0.013[5] mas/yr
Parallax (π)131.1013 ± 0.0270[5] mas
Distance24.878 ± 0.005 ly
(7.628 ± 0.002 pc)
Details
Mass0.526[6] M☉
Radius0.611±0.043[6] R☉
Luminosity (bolometric)0.043[6] L☉
Surface gravity (log g)4.59[6] cgs
Temperature2,901[7] - 3,727[3] K
Metallicity [Fe/H]−0.07±0.07[3] dex
Rotation28.0±2.9[8]
Rotational velocity (v sin i)2.00[9] km/s
Age8.25[10] Gyr
Other designations
BD+11 2576, HIP 65859, LTT 13925, Ross 490, TYC 895-317-1, 2MASS J13295979+1022376, Gaia EDR3 3738099879558957952[1]
Database references
SIMBADdata

Gliese 514, also known as BD+11 2576 or HIP 65859, is a M-type main-sequence star, in the constellation Virgo 24.85 light-years away from the Sun. The proximity of Gliese 514 to the Sun was known exactly since 1988.[11]

Gliese 514's metallicity Fe/H index is largely unknown, with median values from -0.4 to +0.18 reported in the literature. This discrepancy is due to peculiarities of the stellar spectrum of Gliese 514. The spectrum peculiarities also affect the accuracy of the star's temperature measurement,[9] with reported values as low as 2901 K.[7] The spectrum of Gliese 514 shows emission lines,[2] but the star itself has a low starspot activity.[12]

Multiplicity surveys did not detect any stellar companions as of 2020.[13]

The Sun is currently calculated to be passing through the tidal tail of Gliese 514`s Oort cloud. Thus, future interstellar objects passing through Solar system may originate from Gliese 514.[14]

Planetary system

The existence of a planet on a 15-day orbit around Gliese 514 was suspected since 2019.[15] However, that planet was not confirmed. Instead, in 2022, one Super-Earth planet, named Gliese 514 b, was discovered on an eccentric 140-day orbit by the radial velocity method. The planetary orbit partially lies within the habitable zone of the parent star with planetary equilibrium temperature, averaged along orbit, equal to 202±11 K.[8]

The infrared excess of the star also indicates the possible presence of a debris disk in the system, albeit at a low signal to noise ratio.[16]

The Gliese 514 planetary system[8]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b >5.2±0.9 M⊕ 0.422+0.014−0.015 140.43±0.41 0.45+0.15−0.14 — —

References

  1. ↑ 1.0 1.1 1.2 "BD+11 2576". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=BD%2B11+2576. 
  2. ↑ 2.0 2.1 Lindegren, Lennart; Dravins, Dainis (2021), "Astrometric radial velocities for nearby stars", Astronomy & Astrophysics 652: A45, doi:10.1051/0004-6361/202141344, Bibcode: 2021A&A...652A..45L 
  3. ↑ 3.0 3.1 3.2 3.3 Lindgren, Sara; Heiter, Ulrike (2017), "Metallicity determination of M dwarfs", Astronomy & Astrophysics 604: A97, doi:10.1051/0004-6361/201730715, Bibcode: 2017A&A...604A..97L 
  4. ↑ Manara, C. F. et al. (2021), "PENELLOPE: The ESO data legacy program to complement the Hubble UV Legacy Library of Young Stars (ULLYSES)", Astronomy & Astrophysics 650: A196, doi:10.1051/0004-6361/202140639 
  5. ↑ 5.0 5.1 5.2 Brown, A. G. A. (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics 649: A1. doi:10.1051/0004-6361/202039657. Bibcode: 2021A&A...649A...1G.  Gaia EDR3 record for this source at VizieR.
  6. ↑ 6.0 6.1 6.2 6.3 Berger, D. H.; Gies, D. R.; McAlister, H. A.; Brummelaar, T. A. ten; Henry, T. J.; Sturmann, J.; Sturmann, L.; Turner, N. H. et al. (2006), "First Results from the CHARA Array. IV. The Interferometric Radii of Low‐Mass Stars", The Astrophysical Journal 644 (1): 475–483, doi:10.1086/503318, Bibcode: 2006ApJ...644..475B 
  7. ↑ 7.0 7.1 Ghosh, Samrat; Ghosh, Supriyo; Das, Ramkrishna; Mondal, Soumen; Khata, Dhrimadri (2020), "Understanding the physical properties of young M dwarfs: NIR spectroscopic studies", Monthly Notices of the Royal Astronomical Society 493 (3): 4533–4550, doi:10.1093/mnras/staa427, Bibcode: 2020MNRAS.493.4533K 
  8. ↑ 8.0 8.1 8.2 Damasso, M. et al. (2022), "A quarter century of spectroscopic monitoring of the nearby M dwarf Gl 514", Astronomy & Astrophysics 666: A187, doi:10.1051/0004-6361/202243522 
  9. ↑ 9.0 9.1 Olander, T.; Heiter, U.; Kochukhov, O. (2021), "Comparative high-resolution spectroscopy of M dwarfs: Exploring non-LTE effects", Astronomy & Astrophysics 649: A103, doi:10.1051/0004-6361/202039747, Bibcode: 2021A&A...649A.103O 
  10. ↑ Maldonado, J.; Micela, G.; Baratella, M.; d'Orazi, V.; Affer, L.; Biazzo, K.; Lanza, A. F.; Maggio, A. et al. (2020). "HADES RV programme with HARPS-N at TNG. XII. The abundance signature of M dwarf stars with planets". Astronomy and Astrophysics 644: A68. doi:10.1051/0004-6361/202039478. Bibcode: 2020A&A...644A..68M. 
  11. ↑ Determinations of the parallaxes of BD +11 2576 and BD +18 683
  12. ↑ Reiners, A. (2007), "The narrowest M-dwarf line profiles and the rotation-activity connection at very slow rotation", Astronomy and Astrophysics 467 (1): 259, doi:10.1051/0004-6361:20066991, Bibcode: 2007A&A...467..259R 
  13. ↑ Lamman, Claire; Baranec, Christoph; Berta-Thompson, Zachory K.; Law, Nicholas M.; Schonhut-Stasik, Jessica; Ziegler, Carl; Salama, Maïssa; Jensen-Clem, Rebecca et al. (2020), "Robo-AO M-dwarf Multiplicity Survey: Catalog", The Astronomical Journal 159 (4): 139, doi:10.3847/1538-3881/ab6ef1, Bibcode: 2020AJ....159..139L 
  14. ↑ Portegies Zwart, S. (2021), "Oort cloud Ecology", Astronomy & Astrophysics 647: A136, doi:10.1051/0004-6361/202038888 
  15. ↑ Barnes, J. R.; et al. (2019-06-11). "Frequency of planets orbiting M dwarfs in the Solar neighbourhood". arXiv:1906.04644 [astro-ph.EP].
  16. ↑ Tanner, Angelle; Plavchan, Peter; Bryden, Geoff; Kennedy, Grant; Matrá, Luca; Cronin-Coltsmann, Patrick; Lowrance, Patrick; Henry, Todd et al. (2020), "Herschel Observations of Disks around Late-type Stars", Publications of the Astronomical Society of the Pacific 132 (1014): 084401, doi:10.1088/1538-3873/ab895f, Bibcode: 2020PASP..132h4401T 



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