Langbahn Team – Weltmeisterschaft

HD 211415

HD 211415 A/B
Observation data
Epoch J2000      Equinox J2000
Constellation Grus
Right ascension 22h 18m 15.61403s[1]
Declination –53° 37′ 37.4640″[1]
Apparent magnitude (V) 5.33[2]/9.9[3]
Characteristics
Spectral type G0V[4] + MV
U−B color index +0.06[2]
B−V color index +0.61[2]
Astrometry
Radial velocity (Rv)−12.68±0.17[5] km/s
Proper motion (μ) RA: +438.75[1] mas/yr
Dec.: –632.46[1] mas/yr
Parallax (π)72.54 ± 0.36 mas[1]
Distance45.0 ± 0.2 ly
(13.79 ± 0.07 pc)
Absolute magnitude (MV)4.69[6]
Details
HD 211415 A
Mass0.941±0.016[7] M☉
Surface gravity (log g)4.42±0.03[7] cgs
Temperature5,864±18[7] K
Metallicity [Fe/H]−0.21±0.01[7] dex
Rotational velocity (v sin i)0.32[8] km/s
Age2.6–4.1[9] Gyr
HD 211415 B
Mass0.59[10] M☉
Other designations
CD -54°9222, GCTP 5395.00, GJ 853 A, HD 211415, HIP 110109, HR 8501, LHS 3790, LFT 1702, LTT 8943, SAO 247400.[11]
Database references
SIMBADdata

HD 211415 is a double star in the constellation Grus. With an apparent visual magnitude of 5.33,[2] it is visible to the naked eye. The annual parallax shift is 72.54 mas, which yields a distance estimate of 45 light years. It has a relatively high proper motion, traversing the celestial sphere at the rate of 93.4 mas per year,[12] and is moving closer to the Sun with a radial velocity of −13 km/s.[5]

As of 1994, the two members of this system have an angular separation of 2.884″ along a position angle of 34.935°.[3] Their projected separation is 39.8 AU.[12] The pair are most likely gravitationally-bound with an orbit is probably being viewed nearly edge-on and a semimajor axis of around 100 AU.[13]

HD 211415 was identified in September 2003 by astrobiologist Margaret Turnbull from the University of Arizona in Tucson as one of the most promising nearby candidates for hosting life based on her analysis of the HabCat list of stars.[14] It is a G-type main-sequence star with a stellar classification of G0 V.[4]

References

  1. ^ a b c d e van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357, S2CID 18759600.
  2. ^ a b c d Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV Data, SIMBAD, Bibcode:1986EgUBV........0M.
  3. ^ a b Poveda, A.; et al. (April 1994), "Statistical studies of visual double and multiple stars. II. A catalogue of nearby wide binary and multiple systems", Revista Mexicana de Astronomía y Astrofísica, 28 (1): 43–89, Bibcode:1994RMxAA..28...43P. See pp. 80–81.
  4. ^ a b Gray, R. O.; et al. (2006). "Contributions to the Nearby Stars (NStars) Project: spectroscopy of stars earlier than M0 within 40 pc-The Southern Sample". The Astronomical Journal. 132 (1): 161–70. arXiv:astro-ph/0603770. Bibcode:2006AJ....132..161G. doi:10.1086/504637. S2CID 119476992.
  5. ^ a b Maldonado, J.; et al. (October 2010), "A spectroscopy study of nearby late-type stars, possible members of stellar kinematic groups", Astronomy and Astrophysics, 521: A12, arXiv:1007.1132, Bibcode:2010A&A...521A..12M, doi:10.1051/0004-6361/201014948, S2CID 119209183
  6. ^ Holmberg, J.; et al. (July 2009), "The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics", Astronomy and Astrophysics, 501 (3): 941–947, arXiv:0811.3982, Bibcode:2009A&A...501..941H, doi:10.1051/0004-6361/200811191, S2CID 118577511.
  7. ^ a b c d Tsantaki, M.; et al. (July 2013), "Deriving precise parameters for cool solar-type stars. Optimizing the iron line list", Astronomy & Astrophysics, 555: A150, arXiv:1304.6639, Bibcode:2013A&A...555A.150T, doi:10.1051/0004-6361/201321103, S2CID 118388752.
  8. ^ Martínez-Arnáiz, R.; et al. (September 2010). "Chromospheric activity and rotation of FGK stars in the solar vicinity. An estimation of the radial velocity jitter" (PDF). Astronomy and Astrophysics. 520: A79. arXiv:1002.4391. Bibcode:2010A&A...520A..79M. doi:10.1051/0004-6361/200913725. S2CID 43455849. Archived from the original (PDF) on 2017-09-22. Retrieved 2018-11-04.
  9. ^ Mamajek, Eric E.; Hillenbrand, Lynne A. (November 2008). "Improved Age Estimation for Solar-Type Dwarfs Using Activity-Rotation Diagnostics". The Astrophysical Journal. 687 (2): 1264–1293. arXiv:0807.1686. Bibcode:2008ApJ...687.1264M. doi:10.1086/591785. S2CID 27151456.
  10. ^ Tokovinin, Andrei (April 2014), "From Binaries to Multiples. II. Hierarchical Multiplicity of F and G Dwarfs", The Astronomical Journal, 147 (4): 14, arXiv:1401.6827, Bibcode:2014AJ....147...87T, doi:10.1088/0004-6256/147/4/87, S2CID 56066740, 87.
  11. ^ "HD 45088 -- Variable of BY Dra type", SIMBAD Astronomical Database, Centre de Données astronomiques de Strasbourg, retrieved 2015-04-17.
  12. ^ a b Tokovinin, A.; Kiyaeva, O. (2015), "Eccentricity distribution of wide binaries", Monthly Notices of the Royal Astronomical Society, 456 (2): 2070, arXiv:1512.00278, Bibcode:2016MNRAS.456.2070T, doi:10.1093/mnras/stv2825, S2CID 1615080.
  13. ^ Krist, John E.; et al. (October 2010), "HST and Spitzer Observations of the HD 207129 Debris Ring", The Astronomical Journal, 140 (4): 1051−1061, arXiv:1008.2793, Bibcode:2010AJ....140.1051K, doi:10.1088/0004-6256/140/4/1051, S2CID 43979052.
  14. ^ "Astronomer Announces Shortlist Of Stellar Candidates For Habitable Worlds". Science Daily. 2006-02-21. Retrieved 2006-05-24.
Quelle: https://en.wikipedia.org/wiki/HD_211415