Langbahn Team – Weltmeisterschaft

TYC 9486-927-1

TYC 9486-927-1

A light curve for FT Octantis, plotted from TESS data[1]
Observation data
Epoch J2000      Equinox J2000
Constellation Octans
Right ascension 21h 25m 27.4805s[2]
Declination −81° 38′ 27.692″[2]
Apparent magnitude (V) 11.5 - 12.0[3]
Characteristics
Spectral type M1 V[4]
Variable type BY Dra[3]
Astrometry
Radial velocity (Rv)8.7±4.6[4] km/s
Proper motion (μ) RA: 60.645(46) mas/yr[2]
Dec.: −107.740(48) mas/yr[2]
Parallax (π)29.0266 ± 0.0401 mas[2]
Distance112.4 ± 0.2 ly
(34.45 ± 0.05 pc)
Details
Mass0.53[5] M☉
Radius0.46[6] R☉
Luminosity0.032[6] L☉
Surface gravity (log g)4.3[7] cgs
Temperature3,490[8] K
Metallicity [Fe/H]−1.3[7] dex
Rotation0.541945[3] days
Rotational velocity (v sin i)43.5±1.2[8] km/s
Age10-45[8] Myr
Other designations
2MASS J21252752-8138278, FT Octantis
Database references
SIMBADdata

TYC 9486-927-1 (also known as 2MASS J21252752-8138278) is the primary of a possible trinary star system located at a distance of 34.5 parsecs from Earth in the southern direction in the constellation of Octans. It is a BY Draconis variable, with large starspots causing it to change brightness as it rotates every 13 hours.[3]

TYC 9486-927-1 has rapid rotation and coronal and chromospheric activity suggestive of a young age. Observations and multi-epoch radial velocity data suggest that TYC 9486-927-1 is a single, rapidly rotating star rather than a spectroscopic or tight visual binary. However, it is still possible that TYC 9486-927-1 is an equal mass binary with a face-on orbit and close separation.[4]

The candidate secondary stellar companion is 2MASS J21121598–8128452. It is a red dwarf star of spectral class M5.5. Its projected separation from the primary would be 62,700 AU. The candidate tertiary companion is 2MASS J21192028–8145446 - of spectral class M6 or M7 and at a projected separation of 31,000 AU from the primary.[5]: 7 

Planetary system

The planet 2MASS J21265040-8140293 orbits TYC 9486-927-1 at a projected separation of 7400 AU.[5] With a mass from 11.6 to 15 Jupiter masses, it is considered to be either a brown dwarf, or a giant planet.[9][10]

The TYC 9486-927-1 planetary system
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
2MASS J2126–8140/b 13.3 (± 1.7)[11] MJ 6,900[8] 328 725 000[citation needed] — — —

References

  1. ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
  2. ^ a b c d 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. ^ a b c d Samus, N. N.; et al. (2017). "General Catalogue of Variable Stars". Astronomy Reports. 5.1. 61 (1): 80–88. Bibcode:2017ARep...61...80S. doi:10.1134/S1063772917010085. S2CID 125853869.
  4. ^ a b c Torres, C. A. O.; Quast, G. R.; Da Silva, L.; de la Reza, R.; Melo, C. H. F.; Sterzik, M. (2006). "Search for associations containing young stars (SACY). I. Sample and searching method". Astronomy and Astrophysics. 460 (3): 695. arXiv:astro-ph/0609258. Bibcode:2006A&A...460..695T. doi:10.1051/0004-6361:20065602. S2CID 16080025.
  5. ^ a b c Jones, H R A.; Caballero, J. A.; Beamín, J. C.; Barrado, D.; Sarro, L. M.; Marocco, F.; Smart, R. L. (2019), "The Gaia Ultra-Cool Dwarf Sample – II: Structure at the end of the main sequence", Monthly Notices of the Royal Astronomical Society, 485 (3): 4423–4440, arXiv:1902.07571, Bibcode:2019MNRAS.485.4423S, doi:10.1093/mnras/stz678, S2CID 119421722
  6. ^ a b Gaidos, E.; et al. (September 2014). "Trumpeting M dwarfs with CONCH-SHELL: a catalogue of nearby cool host-stars for habitable exoplanets and life". Monthly Notices of the Royal Astronomical Society. 443 (3): 2561–2578. arXiv:1406.7353. Bibcode:2014MNRAS.443.2561G. doi:10.1093/mnras/stu1313. S2CID 119234492.
  7. ^ a b Steinmetz, M.; et al. (2020). "VizieR Online Data Catalog: RAVE 6th data release (Steinmetz+, 2020)". Vizier Online Data Catalog. Bibcode:2020yCat.3283....0S.
  8. ^ a b c d Deacon, N. R.; Schlieder, J. E.; Murphy, S. J. (2016). "A nearby young M dwarf with a wide, possibly planetary-mass companion". Monthly Notices of the Royal Astronomical Society. 457 (3): 3191. arXiv:1601.06162. Bibcode:2016MNRAS.457.3191D. doi:10.1093/mnras/stw172. S2CID 18220333.
  9. ^ Gagné, Jonathan; Lafrenière, David; Doyon, René; Malo, Lison; Artigau, Étienne (2014). "BANYAN. II. Very Low Mass and Substellar Candidate Members to Nearby, Young Kinematic Groups with Previously Known Signs of Youth". The Astrophysical Journal. 783 (2): 121. arXiv:1312.5864. Bibcode:2014ApJ...783..121G. doi:10.1088/0004-637X/783/2/121. S2CID 119251619.
  10. ^ Reid, I. Neill; Cruz, Kelle L.; Kirkpatrick, J. Davy; Allen, Peter R.; Mungall, F.; Liebert, James; Lowrance, Patrick; Sweet, Anne (2008). "Meeting the Cool Neighbors. X. Ultracool Dwarfs from the 2MASS All-Sky Data Release". The Astronomical Journal. 136 (3): 1290. arXiv:0806.3413. Bibcode:2008AJ....136.1290R. doi:10.1088/0004-6256/136/3/1290.
  11. ^ "Planet 2MASS J2126-8140". Extrasolar Planets Encyclopaedia. Retrieved 2016-01-27.
Quelle: https://en.wikipedia.org/wiki/TYC_9486-927-1