Lacaille_9352

Lacaille 9352

Lacaille 9352

Star in the constellation Piscis Austrinus

Lacaille 9352 (Lac 9352) is a red dwarf star in the southern constellation of Piscis Austrinus. With an apparent visual magnitude of 7.34,[2] this star is too faint to be viewed with the naked eye except possibly under excellent seeing conditions. Parallax measurements place it at a distance of about 10.74 light-years (3.29 parsecs) from Earth.[1] It is the eleventh closest star system to the Solar System[14] and is the closest star in the constellation Piscis Austrinus. The ChView simulation[15] shows that its closest neighbour is the EZ Aquarii triple star system at about 4.1 ly away.

Quick Facts Observation data Epoch J2000 Equinox J2000, Constellation ...

Properties

This star has the fourth highest known proper motion,[16] (which was first noticed by Benjamin Gould in 1881[17]) moving a total of 6.9 arcseconds per year. However, this is still a very small movement overall, as there are 3,600 arcseconds in a degree of arc. The space velocity components of this star are (U, V, W) = (−93.9, −14.1, −51.4) km/s.[18] If the radial velocity (Vr) equals +9.7 km/s then about 2,700 years ago Lacaille 9352 was at its minimal distance of approximately 10.63 ly (3.26 pc) from the Sun.[19]

The spectrum of Lacaille 9352 places it at a stellar classification of M0.5V,[3] indicating it is a type of main sequence star known as a red dwarf. This was the first red dwarf star to have its angular diameter measured,[20] with the physical diameter being about 47% of the Sun's radius.[9] It has around half the mass of the Sun[3] and the outer envelope has an effective temperature of about 3,670 K.[9]

Planetary system

In June 2020, two super-Earth planets were reported, as well as a third signal with a period of 50.7 days that may be due to stellar activity—however, if this planet is real it may be located within the habitable zone. They were detected using the radial velocity method from observations with HARPS in Chile and HIRES in Hawaii.[21][22]

More information Companion (in order from star), Mass ...

See also

References

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    Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
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    Murdin, Paul, ed. (November 2000). "Lacaille 9352". Encyclopedia of Astronomy and Astrophysics. Bristol: Institute of Physics Publishing. Bibcode:2000eaa..bookE5158.. doi:10.1888/0333750888/5158. ISBN 0333750888. absolute magnitude is 9.8
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    Pineda, J. Sebastian; et al. (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.
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  14. [14]
    Research Consortium on Nearby Stars. "The One Hundred Nearest Star Systems". Georgia State University. Archived from the original on 2012-05-13. Retrieved 2010-01-20.
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    "Solstation and ChView". Retrieved 2010-04-20.
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  17. [17]
    Gould, B. A. (1881). "Corrigenda in the Uranometria Argentina. Star with large proper motion". Astronomische Nachrichten. 100 (1): 7–10. Bibcode:1881AN....100....7G. doi:10.1002/asna.18811000104.
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    "ARICNS star page of Lacaille 9352". Astronomisches Rechen-Institut Heidelberg. Archived from the original on 2012-09-16. Retrieved 2010-04-16.
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  21. [21]
    Jeffers, S. V.; Dreizler, S.; Barnes, J. R.; Haswell, C. A.; Nelson, R. P.; Rodríguez, E.; López-González, M. J.; Morales, N.; Luque, R.; et al. (2020), "A multiple planet system of super-Earths orbiting the brightest red dwarf star GJ887", Science, 368 (6498): 1477–1481, arXiv:2006.16372, Bibcode:2020Sci...368.1477J, doi:10.1126/science.aaz0795, PMID 32587019, S2CID 220075207
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    Witze, Alexandra (2020). "Why boring could be good for this star's two intriguing planets". Nature. doi:10.1038/d41586-020-01905-5. PMID 34168349. S2CID 220507688. Retrieved 2020-06-30.
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