Ross 47

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Ross 47
Orion constellation map.svg
Red pog.png
Ross 47
Location of Ross 47 in the constellation Orion

Observation data
Epoch J2000.0        Equinox J2000.0
Constellation Orion [1]
Right ascension 05h 42m 09.26769s [2]
Declination +12° 29′ 21.6048″ [2]
Apparent magnitude  (V)+11.48 - 11.55 [3]
Characteristics
Evolutionary stage red dwarf
Spectral type M4V [4]
U−B color index +14.264
B−V color index +13.130
Variable type BY Dra [3]
Astrometry
Radial velocity (Rv)106.06±0.18 [2] km/s
Proper motion (μ)RA: +1,997.342 [2] mas/yr
Dec.: −1569.63 [2] mas/yr
Parallax (π)172.6762±0.0286  mas [2]
Distance 18.888 ± 0.003  ly
(5.7912 ± 0.0010  pc)
Absolute magnitude  (MV)+12.73 [1]
Details
Mass 0.218±0.005 [5]   M☉
Radius 0.238±0.009 [5]   R☉
Luminosity 0.006288±0.000094 [5]   L☉
Surface gravity (log g)4.44 [2]   cgs
Temperature 3,334+67
−63 [5]   K
Metallicity [Fe/H]−0.19±0.17 [6]   dex
Rotation 170 [7]
Rotational velocity (v sin i)3.1 [8]  km/s
Age 7.1 [9]   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 [10]
Database references
SIMBAD data

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 from Earth.

A visual band light curve for V1352 Orionis, adapted from Weis (1994) V1352OriLightCurve.png
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. [5] It is a BY Draconis variable, a star which whose brightness varies across its rotation, having multiple starspots that contribute to the brightness variation. [3] Its apparent magnitude varies from +11.48 to 11.55. [3] Ross 47 was given the variable star designation V1352 Orionis in 1997. [12]

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.
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