Ross 47

Ross 47
Ross 47 is located in the constellation Orion
Ross 47 is located in the constellation Orion
Ross 47
Location of Ross 47 in the constellation Orion

Observation data
Epoch J2000.0      Equinox ICRS
Constellation Orion
Right ascension 05h 42m 09.26769s
Declination +12° 29′ 21.6048″
Apparent magnitude (V) +11.48 - 11.55
Characteristics
Evolutionary stage red dwarf
Spectral type M4V
U−B color index +14.264
B−V color index +13.130
Variable type BY Dra
Astrometry
Radial velocity (Rv)106.06±0.18 km/s
Proper motion (μ) RA: +1,997.342 mas/yr
Dec.: −1569.63 mas/yr
Parallax (π)172.6762±0.0286 mas
Distance18.888 ± 0.003 ly
(5.7912 ± 0.0010 pc)
Absolute magnitude (MV)+12.73
Details
Mass0.218±0.005 M☉
Radius0.238±0.009 R☉
Luminosity0.006288±0.000094 L☉
Surface gravity (log g)4.44 cgs
Temperature3,334+67
−63 K
Metallicity [Fe/H]−0.19±0.17 dex
Rotation170
Rotational velocity (v sin i)3.1 km/s
Age7.1 Gyr
Other designations
V1352 Ori, GJ 213, HIP 26857, Ci 20 344, G 102-22, LFT 425, LHS 31, LTT 11704, NLTT 15489, Ross 47, TYC 722-455-1, 2MASS J05420897+1229252
Database references
SIMBADdata

Ross 47 is a variable star of spectral type M4 located in the constellation Orion. Based on parallax measurements, it lies 18.888 light-years (5.791 parsecs) from Earth.

A visual band light curve for V1352 Orionis, adapted from Weis (1994)

Ross 47 is a small red dwarf with 23.8% of the Sun's size, and 6% of its luminosity. Its effective temperature is much cooler than the Sun's, about 3,330 K. It is a BY Draconis variable, a star which whose brightness varies across its rotation, having multiple starspots that contribute to the brightness variation. Its apparent magnitude varies from +11.48 to 11.55. Ross 47 was given the variable star designation V1352 Orionis in 1997.

References

  1. 1 2 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. XHIP record for this object at VizieR.
  2. 1 2 3 4 5 6 7 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. 1 2 3 4 Samus, N. N.; et al. (2017). "General Catalogue of Variable Stars". Astronomy Reports. GCVS 5.1. 61 (1): 80–88. Bibcode:2017ARep...61...80S. doi:10.1134/S1063772917010085. S2CID 125853869.
  4. ↑ Kirkpatrick, J. Davy; Henry, Todd J.; McCarthy, Donald W. Jr. (1991). "A standard stellar spectral sequence in the red/near-infrared - Classes K5 to M9". Astrophysical Journal Supplement. 77: 417. Bibcode:1991ApJS...77..417K. doi:10.1086/191611.
  5. 1 2 3 4 5 Pineda, J. Sebastian; Youngblood, Allison; France, Kevin (September 2021). "The M-dwarf Ultraviolet Spectroscopic Sample. I. Determining Stellar Parameters for Field Stars". The Astrophysical Journal. 918 (1): 23. arXiv:2106.07656. Bibcode:2021ApJ...918...40P. doi:10.3847/1538-4357/ac0aea. S2CID 235435757. 40.
  6. ↑ Antoniadis-Karnavas, A.; Sousa, S. G.; Delgado-Mena, E.; Santos, N. C.; Teixeira, G. D. C.; Neves, V. (2020), "ODUSSEAS: A machine learning tool to derive effective temperature and metallicity for M dwarf stars", Astronomy & Astrophysics, 636: A9, arXiv:2002.09367, Bibcode:2020A&A...636A...9A, doi:10.1051/0004-6361/201937194, S2CID 211252698
  7. ↑ Astudillo-Defru, N.; Delfosse, X.; Bonfils, X.; Forveille, T.; Lovis, C.; Rameau, J. (2017). "Magnetic activity in the HARPS M dwarf sample. The rotation-activity relationship for very low-mass stars through R'HK". Astronomy and Astrophysics. 600: 600. arXiv:1610.09007. Bibcode:2017A&A...600A..13A. doi:10.1051/0004-6361/201527078. S2CID 119237202.
  8. ↑ Hojjatpanah, S.; Oshagh, M.; Figueira, P.; Santos, N. C.; Amazo-Gómez, E. M.; Sousa, S. G.; Adibekyan, V.; Akinsanmi, B.; Demangeon, O.; Faria, J.; Gomes Da Silva, J.; Meunier, N. (2020). "The correlation between photometric variability and radial velocity jitter. Based on TESS and HARPS observations". Astronomy and Astrophysics. 639: 639. arXiv:2005.10105. Bibcode:2020A&A...639A..35H. doi:10.1051/0004-6361/202038035. S2CID 218719951.
  9. ↑ Maldonado, J.; Micela, G.; Baratella, M.; d'Orazi, V.; Affer, L.; Biazzo, K.; Lanza, A. F.; Maggio, A.; González Hernández, J. I.; Perger, M.; Pinamonti, M.; Scandariato, G.; Sozzetti, A.; Locci, D.; Di Maio, C.; Bignamini, A.; Claudi, R.; Molinari, E.; Rebolo, R.; Ribas, I.; Toledo-Padrón, B.; Covino, E.; Desidera, S.; Herrero, E.; Morales, J. C.; Suárez-Mascareño, A.; Pagano, I.; Petralia, A.; Piotto, G.; Poretti, E. (2020). "HADES RV programme with HARPS-N at TNG. XII. The abundance signature of M dwarf stars with planets". Astronomy and Astrophysics. 644: A68. arXiv:2010.14867. Bibcode:2020A&A...644A..68M. doi:10.1051/0004-6361/202039478. S2CID 260555994.
  10. ↑ "Ross 47". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 16 February 2021.
  11. ↑ Weis, Edward W. (March 1994). "Long Term Variability in Dwarf M Stars". Astronomical Journal. 107 (3): 1135. Bibcode:1994AJ....107.1135W. doi:10.1086/116925. Retrieved 7 September 2024.
  12. ↑ Kazarovets, E. V.; Samus, N. N. (April 1997). "The 73rd Name-List of Variable Stars". Information Bulletin on Variable Stars. 4471 (4471): 1. Bibcode:1997IBVS.4471....1K. Retrieved 7 September 2024.