astro.wikisort.org - StarLambda Serpentis, Latinized from λ Serpentis, is a star in the constellation Serpens, in its head (Serpens Caput). It has an apparent visual magnitude of 4.43,[2] making it visible to the naked eye. Based upon parallax measurements, this star lies at a distance of about 38.9 light-years (11.9 parsecs) from Earth.[1] Lambda Serpentis is moving toward the Solar System with a radial velocity of 66.4 km s−1.[4] In about 166,000 years, this system will make its closest approach of the Sun at a distance of 7.371 ± 0.258 light-years (2.260 ± 0.079 parsecs), before moving away thereafter.[12]
G-type star in the constellation Serpens
Lambda Serpentis
Location of λ Serpentis (circled) |
Observation data Epoch J2000 Equinox J2000 |
Constellation |
Serpens |
Right ascension |
15h 46m 26.61423s[1] |
Declination |
+07° 21′ 11.0475″[1] |
Apparent magnitude (V) |
4.43[2] |
Characteristics |
Spectral type |
G0 V[3] |
U−B color index |
+0.11[2] |
B−V color index |
+0.60[2] |
Variable type |
Suspected |
Astrometry |
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Radial velocity (Rv) | −66.4[4] km/s |
Proper motion (μ) | RA: −224.0±0.2 mas/yr[1] Dec.: −69.8±0.3 mas/yr[1] |
Parallax (π) | 83.92 ± 0.15 mas[1] |
Distance | 38.87 ± 0.07 ly (11.92 ± 0.02 pc) |
Absolute magnitude (MV) | 4.01[5] |
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Details |
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Mass | 1.14[6] M☉ |
Radius | 1.060±0.152[7] R☉ |
Luminosity | 1.94[6] L☉ |
Surface gravity (log g) | 4.09[8] cgs |
Temperature | 5,884±4.4[9] K |
Metallicity [Fe/H] | −0.03[8] dex |
Rotational velocity (v sin i) | 3[10] km/s |
Age | 3.8–6.7[11] Gyr |
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Other designations |
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Database references |
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SIMBAD | data |
This star is 6% larger and 14% more massive than the Sun, although it has a similar stellar classification.[1] It is shining with nearly double the Sun's luminosity and this energy is being radiated from the star's outer atmosphere at an effective temperature of 5,884 K.[9] A periodicity of 1837 days (5.03 years) was suspected by Morbey & Griffith (1987),[13] but it is probably bound to stellar activity. However, McDonald Observatory team has set limits to the presence of one or more exoplanets[13] around Lambda Serpentis with masses between 0.16 and 2 Jupiter masses and average separations spanning between 0.05 and 5.2 Astronomical Units.
Planetary system
In 2020, a candidate planet was detected orbiting Lambda Serpentis (HD 141004). With a minimum mass of 0.043 MJ (13.6 MEarth) and an orbital period of 15 days, this would most likely be a hot Neptune.[14] The discovery of planet was confirmed in 2021.[15]
The Lambda Serpentis planetary system[15]
Companion (in order from star) |
Mass |
Semimajor axis (AU) |
Orbital period (days) |
Eccentricity |
Inclination |
Radius |
b |
≥ 0.0428+0.0047 −0.0045 MJ |
0.1238±0.002 |
15.5083+0.0016 −0.0018 |
0.16+0.11 −0.10 |
— |
— |
References
- 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.
- Johnson, H. L.; Morgan, W. W. (1953). "Fundamental stellar photometry for standards of spectral type on the revised system of the Yerkes spectral atlas". Astrophysical Journal. 117: 313–352. Bibcode:1953ApJ...117..313J. doi:10.1086/145697. S2CID 18072563.
- "lam Ser -- Spectroscopic binary". SIMBAD. Centre de Données astronomiques de Strasbourg. Retrieved 2010-12-15.
- Wilson, Ralph Elmer (1953). "General Catalogue of Stellar Radial Velocities". Carnegie Institute Washington D.C. Publication. Washington: Carnegie Institution of Washington. Bibcode:1953GCRV..C......0W.
- Holmberg, J.; et al. (July 2009), "The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics", Astronomy and Astrophysics, 501 (3): 941–947, arXiv:0811.3982, Bibcode:2009A&A...501..941H, doi:10.1051/0004-6361/200811191, S2CID 118577511.
- Valenti, J. A.; Fishcer, D. A. (2005). "Spectroscopic Properties of Cool Stars (SPOCS). I. 1040 F, G, and K Dwarfs from Keck, Lick, and AAT Planet Search Programs". Astrophysical Journal Supplement Series. 159 (1): 141–166. Bibcode:2005ApJS..159..141V. doi:10.1086/430500.
- van Belle, Gerard T.; von Braun, Kaspar (2009). "Directly Determined Linear Radii and Effective Temperatures of Exoplanet Host Stars". The Astrophysical Journal. 694 (2): 1085–1098. arXiv:0901.1206. Bibcode:2009ApJ...694.1085V. doi:10.1088/0004-637X/694/2/1085. S2CID 18370219.
- Fuhrmann, Klaus (October 1998). "Nearby stars of the Galactic disk and halo". Astronomy and Astrophysics. 338: 161–183. Bibcode:1998A&A...338..161F.
- Kovtyukh; Soubiran, C.; Belik, S. I.; Gorlova, N. I. (2003). "High precision effective temperatures for 181 F-K dwarfs from line-depth ratios". Astronomy and Astrophysics. 411 (3): 559–564. arXiv:astro-ph/0308429. Bibcode:2003A&A...411..559K. doi:10.1051/0004-6361:20031378. S2CID 18478960.
- Bernacca, P. L.; Perinotto, M. (1970). "A catalogue of stellar rotational velocities". Contributi Osservatorio Astronomico di Padova in Asiago. 239 (1): 1. Bibcode:1970CoAsi.239....1B.
- Mamajek, Eric E.; Hillenbrand, Lynne A. (November 2008). "Improved Age Estimation for Solar-Type Dwarfs Using Activity-Rotation Diagnostics". The Astrophysical Journal. 687 (2): 1264–1293. arXiv:0807.1686. Bibcode:2008ApJ...687.1264M. doi:10.1086/591785. S2CID 27151456.
- Dybczyński, P. A. (April 2006), "Simulating observable comets. III. Real stellar perturbers of the Oort cloud and their output", Astronomy and Astrophysics, 449 (3): 1233–1242, Bibcode:2006A&A...449.1233D, doi:10.1051/0004-6361:20054284
- Morbey, C. L.; Griffith, R. F. (1987). "On the reality of certain spectroscopic orbits". Astrophysical Journal. 317 (1): 343–352. Bibcode:1987ApJ...317..343M. doi:10.1086/165281.
- Hirsch, Lea A.; et al. (2021), "Understanding the Impacts of Stellar Companions on Planet Formation and Evolution: A Survey of Stellar and Planetary Companions within 25 pc", The Astronomical Journal, 161 (3): 134, arXiv:2012.09190, Bibcode:2020arXiv201209190H, doi:10.3847/1538-3881/abd639, S2CID 229297873.
- Rosenthal, Lee J.; Fulton, Benjamin J.; Hirsch, Lea A.; Isaacson, Howard T.; Howard, Andrew W.; Dedrick, Cayla M.; Sherstyuk, Ilya A.; Blunt, Sarah C.; Petigura, Erik A.; Knutson, Heather A.; Behmard, Aida; Chontos, Ashley; Crepp, Justin R.; Crossfield, Ian J. M.; Dalba, Paul A.; Fischer, Debra A.; Henry, Gregory W.; Kane, Stephen R.; Kosiarek, Molly; Marcy, Geoffrey W.; Rubenzahl, Ryan A.; Weiss, Lauren M.; Wright, Jason T. (2021), "The California Legacy Survey. I. A Catalog of 178 Planets from Precision Radial Velocity Monitoring of 719 Nearby Stars over Three Decades", The Astrophysical Journal Supplement Series, 255: 8, arXiv:2105.11583, doi:10.3847/1538-4365/abe23c, S2CID 235186973
Further reading
Serpens constellation |
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Stars (list) | |
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Star clusters | |
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Molecular clouds | |
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Nebulae | |
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Galaxies | NGC |
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- 5910
- 5911
- 5913
- 5919
- 5920
- 5921
- 5926
- 5928
- 5931
- 5936
- 5937
- 5940
- 5942
- 5941
- 5944
- 5951
- 5953
- 5954
- 5952
- 5956
- 5955
- 5957
- 5960
- 5962
- 5964
- 5970
- 5972
- 5975
- 5977
- 5980
- 5983
- 5984
- 5988
- 5991
- 5990
- 5994
- 5996
- 5997
- 6003
- 6004
- 6008
- 6006
- 6007
- 6009
- 6012
- 6010
- 6014
- 6020
- 6017
- 6018
- 6021
- 6022
- 6023
- 6027
- 6027a
- 6027b
- 6027c
- 6027d
- 6027e
- 6029
- 6033
- 6037
- 6036
- 6051
- 6063
- 6065
- 6066
- 6070
- 6080
- 6100
- 6118
- 6172
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Other | |
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Galaxy clusters | |
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Other |
- GRB 970111
- GRB 050813
- GRB 060418
- GRB 060526
- SN 2004dk
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На других языках
- [en] Lambda Serpentis
[es] Lambda Serpentis
Lambda Serpentis (λ Ser / 27 Serpentis / HD 141004 / GJ 598)[1] es una estrella de magnitud aparente +4,43 que forma parte de la constelación de Serpens. Está situada en el centro de Serpens Caput —la cabeza de la serpiente—, a poco más de 1º de Unukalhai (α Serpentis).
Se encuentra a 38,3 años luz de distancia del Sistema Solar.
[ru] Лямбда Змеи
Лямбда Змеи, (англ. Lambda Serpentis) — звезда, которая находится в созвездии Змея на расстоянии около 38,3 световых лет от нас.
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