SCR_1845−6357

SCR 1845−6357

SCR 1845−6357

Star in the constellation Pavo

SCR 1845−6357 is a binary system, 13.1 light-years (4.0 parsecs) away in the constellation Pavo. The primary is a faint red dwarf. It has a brown dwarf companion. The primary red dwarf was discovered in 2004 by Hambly et al.,[8] while the secondary brown dwarf was later discovered in 2006.[9]

Quick Facts Constellation, Right ascension ...

System

Artist's impression of the SCR 1845-6357 stellar system

The primary, SCR 1845−6357A, is a faint (apparent magnitude 17.4)[2] ultra-cool red dwarf with a mass of about 7% of the Sun's. However, the measurements are still preliminary and are subject to change.[5]

SCR 1845–6357, right bottom

This star has been found to possess a brown dwarf companion, designated SCR 1845-6357B. The companion, classified as a T-dwarf, has an observed projected distance of 4.1 AU, an estimated mass between 40 and 50 times the mass of Jupiter, and an estimated effective temperature of 950 K.[3][6] The brown dwarf has a near-IR J-band magnitude of 13.26.[4]

See also

References

  1. [1]
    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.
  2. [2]
    "SCR J1845-6357". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 5 November 2023.
  3. [3]
    Kasper, Markus; Biller, Beth A.; Burrows, Adam; Brandner, Wolfgang; Budaj, Jano; Close, Laird M. (August 2007). "The very nearby M/T dwarf binary SCR 1845-6357". Astronomy and Astrophysics. 471 (2): 655–659. arXiv:0706.3824. Bibcode:2007A&A...471..655K. doi:10.1051/0004-6361:20077881.
  4. [4]
    Chris Gelino; Davy Kirkpatrick; Adam Burgasser. "DwarfArchives.org: Photometry, spectroscopy, and astrometry of M, L, and T dwarfs". caltech.edu. Archived from the original on 2013-11-13. Retrieved 2012-06-10. (main page) Archived 2019-05-11 at the Wayback Machine
  5. [5]
    "THE ONE HUNDRED NEAREST STAR SYSTEMS". Research Consortium On Nearby Stars. Georgia State University. January 1, 2008. Retrieved June 17, 2008.
  6. [6]
    Observed projected distance computed from parallax and observed angular distance.
  7. [7]
    Golovin, Alex; Reffert, Sabine; Just, Andreas; Jordan, Stefan; Vani, Akash; Jahreiß, Hartmut (November 2022). "The Fifth Catalogue of Nearby Stars (CNS5)". Astronomy & Astrophysics. 670: A19. arXiv:2211.01449. Bibcode:2023A&A...670A..19G. doi:10.1051/0004-6361/202244250. S2CID 253264922. Catalogue can be accessed here.
  8. [8]
    Hambly, Nigel C.; Henry, Todd J.; Subasavage, John P.; Brown, Misty A.; Jao, Wei-Chun (2004). "The Solar Neighborhood. VIII. Discovery of New High Proper Motion Nearby Stars Using the SuperCOSMOS Sky Survey". The Astronomical Journal. 128 (1): 437–447. arXiv:astro-ph/0404265. Bibcode:2004AJ....128..437H. doi:10.1086/421748. S2CID 9586813.
  9. [9]
    Biller, B. A.; Kasper, M.; et al. (April 2006). "Discovery of a Brown Dwarf Very Close to the Sun: A Methane-rich Brown Dwarf Companion to the Low-Mass Star SCR 1845-6357". The Astrophysical Journal. 641 (2): L141–L144. arXiv:astro-ph/0601440. Bibcode:2006ApJ...641L.141B. doi:10.1086/504256.
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