39 Leonis is the Flamsteed designation for a star in the zodiac constellation of Leo. It has an apparent visual magnitude of 5.90, so, according to the Bortle scale, it is faintly visible from suburban skies at night. Parallax measurements show an annual parallax shift of 0.0449″,[1] which is equivalent to a distance of around 72.6 ly (22.3 pc) from the Sun.
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Leo |
| Right ascension | 10h 17m 14.538s[1] |
| Declination | +23° 06′ 22.38″[1] |
| Apparent magnitude (V) | 5.81[2]/11.40[3] |
| Characteristics | |
| Spectral type | F6 V[4] + M1[3] |
| U−B color index | –0.05[5] |
| B−V color index | +0.50[5] |
| Astrometry | |
| Radial velocity (Rv) | +37.4[6] km/s |
| Proper motion (μ) | RA: −413.372 mas/yr[1] Dec.: −98.047 mas/yr[1] |
| Parallax (π) | 44.9008 ± 0.0699 mas[1] |
| Distance | 72.6 ± 0.1 ly (22.27 ± 0.03 pc) |
| Details | |
| 39 Leo A | |
| Mass | 0.98[7] M☉ |
| Radius | 0.99[8] R☉ |
| Luminosity | 2.19[7] L☉ |
| Surface gravity (log g) | 4.29±0.14[2] cgs |
| Temperature | 6,118±49[2] K |
| Metallicity [Fe/H] | –0.27[2] dex |
| Rotational velocity (v sin i) | 2.16[9] km/s |
| Age | 6.3[2] Gyr |
| 39 Leo B | |
| Radius | 0.48[8] R☉ |
| Surface gravity (log g) | 4.83±0.05[3] cgs |
| Temperature | 3,740±40[3] K |
| Metallicity [Fe/H] | −0.33±0.06[3] dex |
| Other designations | |
| Database references | |
| SIMBAD | data |
The stellar classification of 39 Leonis is F6 V,[4] indicating it is a main sequence star. It shines with a luminosity more than double that of the Sun, although it has nearly the same mass and size.[7][8] This is a mature star with an estimated age of 6.3 billion years. The abundance of elements other than hydrogen and helium is about half that in the Sun, making this a metal-poor star.[7] The effective temperature of the stellar atmosphere is 6,118 K,[2] giving it the yellow-white hued glow of an F-type star.[11]
Observations made with the Akari satellite at a wavelength of 18 μm show an excess of infrared emission. This suggests the presence of an inner debris disk orbiting the star at a distance greater than four astronomical units (AU). There was no significant excess found at 22 μm.[7]
A companion star is located at an angular separation of 7.72″ along a position angle of 302.7°—this corresponds to a projected separation of 175 AU.[12] It is a red dwarf star with a classification of M1 and an apparent visual magnitude of 11.40.[3]
See also edit
References edit
- ^ a b c d e 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.
- ^ a b c d e f Maldonado, J.; et al. (May 2012). "Metallicity of solar-type stars with debris discs and planets". Astronomy & Astrophysics. 541: A40. arXiv:1202.5884. Bibcode:2012A&A...541A..40M. doi:10.1051/0004-6361/201218800. S2CID 46328823.
- ^ a b c d e f Woolf, Vincent M.; Wallerstein, George (February 2006), "Calibrating M Dwarf Metallicities Using Molecular Indices", The Publications of the Astronomical Society of the Pacific, 118 (840): 218–226, arXiv:astro-ph/0510148, Bibcode:2006PASP..118..218W, doi:10.1086/498459, S2CID 119340035.
- ^ a b Phillips, N. M.; et al. (April 2010), "Target selection for the SUNS and DEBRIS surveys for debris discs in the solar neighbourhood", Monthly Notices of the Royal Astronomical Society, 403 (3): 1089–1101, arXiv:0911.3426, Bibcode:2010MNRAS.403.1089P, doi:10.1111/j.1365-2966.2009.15641.x, S2CID 119262858.
- ^ a b Johnson, H. L.; et al. (1966), "UBVRIJKL photometry of the bright stars", Communications of the Lunar and Planetary Laboratory, 4 (99): 99, Bibcode:1966CoLPL...4...99J.
- ^ Nordström, B.; et al. (May 2004), "The Geneva-Copenhagen survey of the Solar neighbourhood. Ages, metallicities, and kinematic properties of ˜14,000 F and G dwarfs", Astronomy and Astrophysics, 418: 989–1019, arXiv:astro-ph/0405198, Bibcode:2004A&A...418..989N, doi:10.1051/0004-6361:20035959, S2CID 11027621.
- ^ a b c d e Fujiwara, H.; et al. (February 2013), "AKARI/IRC 18 μm survey of warm debris disks", Astronomy and Astrophysics, 550: A15, arXiv:1211.6365, Bibcode:2013A&A...550A..45F, doi:10.1051/0004-6361/201219841, S2CID 1844309.
- ^ a b c Pasinetti-Fracassini, L. E.; et al. (February 2001), "Catalogue of Stellar Diameters (CADARS)", Astronomy and Astrophysics, 367: 521–524, arXiv:astro-ph/0012289, Bibcode:2001A&A...367..521P, doi:10.1051/0004-6361:20000451, S2CID 425754.
- ^ Martínez-Arnáiz, R.; et al. (September 2010), "Chromospheric activity and rotation of FGK stars in the solar vicinity. An estimation of the radial velocity jitter" (PDF), Astronomy and Astrophysics, 520: A79, arXiv:1002.4391, Bibcode:2010A&A...520A..79M, doi:10.1051/0004-6361/200913725, S2CID 43455849, archived from the original (PDF) on 2017-09-22, retrieved 2018-11-04.
- ^ "LTT 12754 -- High proper-motion Star", SIMBAD Astronomical Database, Centre de Données astronomiques de Strasbourg, retrieved 2013-10-13.
- ^ "The Colour of Stars", Australia Telescope, Outreach and Education, Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, archived from the original on March 18, 2012, retrieved 2012-01-16.
- ^ Zapatero-Osorio, María Rosa; Martín, Eduardo L. (May 2004), "A CCD imaging search for wide metal-poor binaries", Astronomy and Astrophysics, 419: 167–180, arXiv:astro-ph/0402310, Bibcode:2004A&A...419..167Z, doi:10.1051/0004-6361:20035907, S2CID 1688885.