Gamma Leonis
  | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Leo |
| Right ascension | 10h 19m 58.35056s[1] |
| Declination | 19° 50′ 29.3468″[1] |
| Apparent magnitude (V) | 2.08 (2.37/3.64)[2] |
| Characteristics | |
| Evolutionary stage | Red clump (both stars)[3] |
| Spectral type | K0III G7III[3] |
| U−B color index | 1.00 |
| B−V color index | 1.14 |
| Variable type | RS CVn[4] |
| Astrometry | |
| Radial velocity (Rv) | −36.24±0.18[5] km/s |
| Proper motion (μ) | RA: 304.30[1] mas/yr Dec.: −154.28[1] mas/yr |
| Parallax (π) | 25.07 ± 0.52 mas[1] |
| Distance | 130 ± 3 ly (39.9 ± 0.8 pc)[1] |
| Absolute magnitude (MV) | −0.27/ 0.98[6] |
| Orbit[3][note 1] | |
| Period (P) | 554±27 yr |
| Semi-major axis (a) | 3.1±0.1″ |
| Eccentricity (e) | 0.93±0.02 |
| Inclination (i) | 41±5° |
| Longitude of the node (Ω) | 143.4[7]° |
| Periastron epoch (T) | 1671.3[7] |
| Details[3] | |
| γ Leo A | |
| Mass | 1.66±0.14 M☉ |
| Radius | 26.08±0.79 R☉ |
| Luminosity | 250 L☉ |
| Surface gravity (log g) | 1.8±0.04 cgs |
| Temperature | 4457±63 K |
| Metallicity [Fe/H] | −0.41±0.03 dex |
| Rotational velocity (v sin i) | 1.41 km/s |
| Age | 1.75±0.43 Gyr |
| γ Leo B | |
| Mass | 1.55±0.08 M☉ |
| Radius | 10.55±0.29 R☉ |
| Luminosity | 63.1 L☉ |
| Surface gravity (log g) | 2.56±0.04 cgs |
| Temperature | 4969±15 K |
| Metallicity [Fe/H] | –0.38 ± 0.02 dex |
| Rotational velocity (v sin i) | 1.62 km/s |
| Age | 2.12±0.33 Gyr |
| Other designations | |
| γ Leo A: γ1 Leonis, HD 89484, HR 4057, SAO 81298 | |
| γ Leo B: γ2 Leonis, HD 89485, HR 4058, SAO 81299 | |
| Position (relative to A)[2] | |
| Component | B |
| Epoch of observation | 1820 – 2022 |
| Angular distance | 3.7" (1820), 4.7" (2022)″ |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
Gamma Leonis (γ Leonis, abbreviated Gamma Leo, γ Leo), also named Algieba /ælˈdʒiːbə/,[8][9] is a binary star system in the constellation of Leo, made up of two red giants. In 2009, a planetary companion around the primary was announced.
Nomenclature
[edit]γ Leonis (Latinised to Gamma Leonis) is the star's Bayer designation. The A and B components of the binary are often referred to as γ1 Leonis and γ2 Leonis, respectively.
It also bore the traditional name Algieba or Al Gieba, which originated from the Arabic الجبهة Al-Jabhah, meaning 'the forehead' (despite this meaning, the star actually appears in the mane of Leo). In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN)[10] to catalog and standardize proper names for stars. The WGSN's first bulletin of July 2016[11] included a table of the first two batches of names approved by the WGSN, which included Algieba for this star.
The star's traditional Latin name was Juba. It is known as 軒轅十二 (the Twelfth Star of Xuanyuan) in Chinese (Xuanyuan is the name of the Yellow Emperor).[citation needed]
Algieba, along with Zeta Leonis, Regulus, Mu Leonis, Epsilon Leonis and Eta Leonis, have collectively been called the Sickle, which is an asterism that marks the head of Leo.[12]
Stellar system
[edit]
The bright binary system in Leo with orange-red and yellow or greenish-yellow components is visible through a modest telescope under good atmospheric conditions. To the naked eye, the Algieba system shines at mid-second magnitude, but a telescope easily splits the pair. The double nature of Gamma Leonis was discovered by William Herschel in 1792.[7]
The brighter component (named Gamma1 Leonis) has an apparent magnitude of 2.28 and is of spectral class K0III. This giant K star has a surface temperature of 4,460 K, 250 times the luminosity of the Sun, and 26 times the Sun's diameter. The companion (named Gamma2 Leonis) has an apparent magnitude of 3.51 and belongs to the spectral class G7III. This giant G star has a temperature of 4,970 K, is 63 times more luminous and 10 times larger than the Sun. Both are more likely red clump giants, evolved stars that have initiated helium ignition at their core. They are estimated to be 2 billion years old and have subsolar metallicites.[3]
The orbital parameters of Gamma Leonis are still uncertain due to the very long orbit. The orbital period is thought to be between 400 and 700 years. Preliminary data show that the stars have an orbital period of 554 years, are visually separated by 3.1' in the sky and have a highly-eccentric (0.93) orbit. Nonetheless, these parameters are contradictory with the physical parameters, by the Kepler's third law, it would imply that the combined mass is of 6.3 M☉. Another data set show parameters that imply a combined mass of 18.6 M☉, even more contradictory with the observed combined mass (3.21 M☉).[3]
Variability
[edit]γ Leonis was a suspected variable star, with a visual magnitude range of 1.84 to 2.03. It is not known which of the two components is variable.[13][14] The American Association of Variable Star Observers mention that it is a RS Canum Venaticorum variable with a smaller range of 1.98 to 2.02.[4] In 1959, the star was mistakenly published as an eclipsing binary due to a typographical error when referring to Y Leonis.[15]
The flare star AD Leonis lies just 5' from γ Leonis.[14] It is unrelated to the pair,[2] and much closer to Earth at a distance of 4.97 parsecs (16.2 ly).[16]
Planetary system
[edit]On November 6, 2009, the discovery of a planetary companion around primary star γ1 Leonis (γ Leonis A) was announced.[7] The radial velocity measurements suggest two additional periodicities of 8.5 and 1,340 days. The former is likely due to stellar pulsation, whereas the latter could be indicative of the presence of an additional planetary companion with 2.14 Jupiter masses, moderate eccentricity (e=0.13) and located at 2.6 AU away from the giant star. Nevertheless, the nature of such a signal is still unclear and further investigations are needed to confirm or rule out an additional substellar companion.
A new study revised the minimum mass for Gamma1 Leonis b to about 10.7 MJ (increased by 20%),[a] based on a larger mass for the host star (1.66 M☉ instead of 1.23 M☉).[3]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | ≥10.7 MJ | 1.19 | 429 | 0.14 | — | — |
| c (unconfirmed) | ≥2.14 MJ | 2.6 | 1,340 | 0.13 | — | — |
Notes
[edit]- ^ The previous mass estimate was 8.78 MJ.
- ^ The orbital parameters are still subject to uncertainites and should be viewed with caution.
References
[edit]- ^ a b c d e f van Leeuwen, F. (November 2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. S2CID 18759600.
- ^ a b c Mason, Brian D.; Wycoff, Gary L.; Hartkopf, William I.; Douglass, Geoffrey G.; Worley, Charles E. (2001). "The 2001 US Naval Observatory Double Star CD-ROM. I. The Washington Double Star Catalog". The Astronomical Journal. 122 (6): 3466–3471. Bibcode:2001AJ....122.3466M. doi:10.1086/323920. ISSN 0004-6256. Gamma Leonis' database entry at VizieR.
- ^ a b c d e f g Takeda, Yoichi (July 2023). "Spectroscopic comparative study of the red giant binary system gamma Leonis A and B". Astrophysics and Space Science. 368 (7): 56. arXiv:2306.16723. Bibcode:2023Ap&SS.368...56T. doi:10.1007/s10509-023-04214-1. ISSN 0004-640X.
- ^ a b "VSX : Detail for gam Leo". AAVSO. Retrieved 2024-06-14.
- ^ Famaey, B.; et al. (January 2005), "Local kinematics of K and M giants from CORAVEL/Hipparcos/Tycho-2 data. Revisiting the concept of superclusters", Astronomy and Astrophysics, 430: 165–186, arXiv:astro-ph/0409579, Bibcode:2005A&A...430..165F, doi:10.1051/0004-6361:20041272, S2CID 17804304
- ^ McWilliam, Andrew (December 1990), "High-resolution spectroscopic survey of 671 GK giants. I - Stellar atmosphere parameters and abundances", Astrophysical Journal Supplement Series, 74: 1075–1128, Bibcode:1990ApJS...74.1075M, doi:10.1086/191527
- ^ a b c d Han, Inwoo; Lee, B. C.; Kim, K. M.; Mkrtichian, D. E.; Hatzes, A. P.; Valyavin, G. (2010). "Detection of a Planetary Companion around the giant star γ-1 Leonis". Astronomy and Astrophysics. 509: A24. arXiv:0911.0968. Bibcode:2010A&A...509A..24H. doi:10.1051/0004-6361/200912536. S2CID 118962986.
- ^ Kunitzsch, Paul; Smart, Tim (2006). A Dictionary of Modern star Names: A Short Guide to 254 Star Names and Their Derivations (2nd rev. ed.). Cambridge, Massachusetts: Sky Pub. ISBN 978-1-931559-44-7.
- ^ "IAU Catalog of Star Names". Retrieved 28 July 2016.
- ^ "IAU Working Group on Star Names (WGSN)". Retrieved 22 May 2016.
- ^ "Bulletin of the IAU Working Group on Star Names, No. 1" (PDF). Retrieved 28 July 2016.
- ^ Proctor, Mary (July 1896), "Evenings with the Stars", Popular Astronomy, 4: 565
- ^ Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1. Bibcode:2009yCat....102025S.
- ^ a b Hoffleit, D.; Warren, W. H., Jr. (1995-11-01). "VizieR Online Data Catalog: Bright Star Catalogue, 5th Revised Ed. (Hoffleit , 1991)". VizieR Online Data Catalog. 5050: V/50. Bibcode:1995yCat.5050....0H.
{{cite journal}}: CS1 maint: multiple names: authors list (link) Gamma Leonis' database entry at VizieR. - ^ "Reports of Observatories". Astronomical Journal. 64: 273. 1959. Bibcode:1959AJ.....64..273.. doi:10.1086/107936.
- ^ 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.
External links
[edit]- Algieba at Jim Kaler's Stars
- Astronomical Reference from Author David Darling
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