Gliese 1

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Gliese 1
Observation data
Epoch J2000       Equinox J2000
Constellation Sculptor
Right ascension 00h 05m 24.4279s [1]
Declination −37° 21′ 26.503″ [1]
Apparent magnitude  (V)8.57 [2]
Characteristics
Spectral type M2V [3]
U−B color index +1.04 [4]
B−V color index +1.46 [4]
Variable type BY Dra [5]
Astrometry
Radial velocity (Rv)+23.6±2 [6]  km/s
Proper motion (μ)RA: +5,633.95 [1]   mas/yr
Dec.: −2,336.69 [1]   mas/yr
Parallax (π)230.0970 ± 0.0362  mas [7]
Distance 14.175 ± 0.002  ly
(4.3460 ± 0.0007  pc)
Absolute magnitude  (MV)10.35 [8]
Details
Mass 0.33±0.07 [9]   M☉
Radius 0.33±0.06 [9]   R☉
Luminosity 0.015+0.007
−0.005 [9]   L☉
Surface gravity (log g)4.91 [9]   cgs
Temperature 3,478±68 [9]   K
Metallicity [Fe/H]−0.26±0.09 [9]   dex
Rotation 60.1±5.7 d [10]
Rotational velocity (v sin i)4.8 [11]  km/s
Age 8.27 [9]   Gyr
Other designations
CD−37°15492, CPD−37°9435, G 267-025, GJ 1, GC  49, GCTP  5817.00, HD  225213, HIP  439, LHS  1, LTT  23, NLTT  134, NSV 15017, SAO  192348 [2]
Database references
SIMBAD data
Sculptor constellation map.svg
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Gliese 1
Location of Gliese 1 in the constellation Sculptor

Gliese 1 is a red dwarf in the constellation Sculptor, which is found in the southern celestial hemisphere. It is one of the closest stars to the Sun, at a distance of 14.2 light years. Because of its proximity to the Earth it is a frequent object of study and much is known about its physical properties and composition. However, with an apparent magnitude of about 8.6 it is too faint to be seen with the naked eye.

Contents

History

This star's high proper motion was first documented by Benjamin Gould in 1885. At that time the star was identified as Cordoba Z.C. 23h 1584. [12] As it lies very close to the origin of the astronomical right ascension coordinates during the 1950 epoch, it became the first star in both the Gliese Catalogue of Nearby Stars and the Luyten Half-Second star catalogues. [13] [14]

Properties

The stellar classification of this star has been rated from M1.5V to M4.0V by various sources. [15] Gliese 1 is estimated to have 33% of the Sun's mass and 33% of the Sun's radius. [9]

This star is suspected of being a BY Draconis-type variable star with the provisional variable star designation NSV 15017. [5] It is also suspected of being a flare star. [16] Like other flare stars, it emits X-rays. [17] The temperatures of the layers of the atmosphere of this star have been measured. [18]

This star has been examined for an orbiting companion using speckle interferometry in the near infrared part of the spectrum. However, no companion was found to a magnitude limit of 10.5 at 1 AU from the primary, out to a magnitude limit of 12.5 at 10 AU. [19] Radial velocity measurements have likewise failed to reveal the presence of a companion orbiting this star. This search excludes a planet with a few Earth masses orbiting in the habitable zone, or a Jupiter-mass planet orbiting at a radius of 1  AU or less. The radial velocity shows little or no variability, with a measurement precision of less than 20 m/s. [20]

The space velocity components of this star are U = +77.2, V = -99.5 and W = −35.6 km/s. [21] It is orbiting through the Milky Way galaxy with an orbital eccentricity of 0.45, and a distance from the galactic core that varies from 3,510 to 9,150 parsecs. By comparison, the Sun is currently 8,500 parsecs from the core. [22] Stars with high peculiar velocities are termed runaway stars. This star has a high peculiar velocity of 111.3 km/s, and the velocity vector for this star may link it with the Tucana-Horologium and/or the AB Doradus stellar associations. [23]

Related Research Articles

<span class="mw-page-title-main">Gliese 570</span> Quaternary star system in the constellation Libra

Gliese 570 is a quaternary star system approximately 19 light-years away. The primary star is an orange dwarf star. The other secondary stars are themselves a binary system, two red dwarfs that orbit the primary star. A brown dwarf has been confirmed to be orbiting in the system. In 1998, an extrasolar planet was thought to orbit the primary star, but it was discounted in 2000.

Gliese 65, also known as Luyten 726-8, is a binary star system that is one of Earth's nearest neighbors, at 8.8 light-years from Earth in the constellation Cetus. The two component stars are both flare stars with the variable star designations BL Ceti and UV Ceti.

<span class="mw-page-title-main">Gliese 876</span> Star in the constellation Aquarius

Gliese 876 is a red dwarf star 15.2 light-years away from Earth in the constellation of Aquarius. It is one of the closest known stars to the Sun confirmed to possess a planetary system with more than two planets, after GJ 1061, YZ Ceti, Tau Ceti, and Wolf 1061; as of 2018, four extrasolar planets have been found to orbit the star. The planetary system is also notable for the orbital properties of its planets. It is the only known system of orbital companions to exhibit a near-triple conjunction in the rare phenomenon of Laplace resonance. It is also the first extrasolar system around a normal star with measured coplanarity. While planets b and c are located in the system's habitable zone, they are giant planets believed to be analogous to Jupiter.

<span class="mw-page-title-main">Gliese 229</span> Star in the constellation Lepus

Gliese 229 is a binary system composed of a red dwarf and the second brown dwarf seen by astronomers, 18.8 light years away in the constellation Lepus. The primary component has 58% of the mass of the Sun, 69% of the Sun's radius, and a very low projected rotation velocity of 1 km/s at the stellar equator.

HD 101930, also known as Gliese 3683, is an orange hued star with an orbiting exoplanet located in the southern constellation Centaurus. It has an apparent magnitude of 8.21, making it faintly visible in binoculars but not to the naked eye. The system is located relatively close at a distance of 98 light years but is receding with a heliocentric radial velocity of 18.4 km/s. It has a relatively large proper motion, traversing the celestial sphere with an angular velocity of 0.320″·yr−1.

HD 114729 is a Sun-like star with an orbiting exoplanet in the southern constellation of Centaurus. Based on parallax measurements, it is located at a distance of 124 light years from the Sun. It is near the lower limit of visibility to the naked eye, having an apparent visual magnitude of 6.68 The system is drifting further away with a heliocentric radial velocity of 26.3 km/s. The system has a relatively high proper motion, traversing the celestial sphere at an angular rate of 0.373″·yr−1.

Gliese 674(GJ 674) is a small red dwarf star with an exoplanetary companion in the southern constellation of Ara. It is too faint to be visible to the naked eye, having an apparent visual magnitude of 9.38 and an absolute magnitude of 11.09. The system is located at a distance of 14.8 light-years from the Sun based on parallax measurements, but is drifting closer with a radial velocity of −2.9 km/s. It is a candidate member of the 200 million year old Castor stream of co-moving stars.

<span class="mw-page-title-main">Gliese 440</span> Star in the constellation Musca

Gliese 440, also known as LP 145-141 or LAWD 37, is an isolated white dwarf located 15.1 light-years from the Solar System in the constellation Musca. It is the fourth closest known white dwarf to the Sun

Gliese 412 is a pair of stars that share a common proper motion through space and are thought to form a binary star system. The pair have an angular separation of 31.4″ at a position angle of 126.1°. They are located 15.8 light-years distant from the Sun in the constellation Ursa Major. Both components are relatively dim red dwarf stars.

Gliese 86 is a K-type main-sequence star approximately 35 light-years away in the constellation of Eridanus. It has been confirmed that a white dwarf orbits the primary star. In 1998 the European Southern Observatory announced that an extrasolar planet was orbiting the star.

HD 181433 is a star with a system of orbiting exoplanets located in the southern constellation of Pavo. With an apparent visual magnitude of 8.40, it is too faint to be visible to the naked eye. It lies at a distance of 88 light years from the Sun based on parallax measurements, and is drifting further away with a radial velocity of +40 km/s. The system shows a high proper motion, traversing the celestial sphere at an angular rate of 0.340 arcsec yr−1.

Gliese 433 is a dim red dwarf star with multiple exoplanetary companions, located in the equatorial constellation of Hydra. The system is located at a distance of 29.6 light-years from the Sun based on parallax measurements, and it is receding with a radial velocity of +18 km/s. Based on its motion through space, this is an old disk star. It is too faint to be viewed with the naked eye, having an apparent visual magnitude of 9.81 and an absolute magnitude of 10.07.

Gliese 163 is a faint red dwarf star with multiple exoplanetary companions in the southern constellation of Dorado. Other stellar catalog names for it include HIP 19394 and LHS 188. It is too faint to be visible to the naked eye, having an apparent visual magnitude of 11.79 and an absolute magnitude of 10.91. This system is located at a distance of 49.4 light-years from the Sun based on parallax measurements. Judging by its space velocity components, it is most likely a thick disk star.

Gliese 221, also known as BD-06 1339, is a star with an exoplanetary companion in the equatorial constellation of Orion. It is too faint to be visible to the naked eye, having an apparent visual magnitude of 9.70 and an absolute magnitude of 8.15. Using parallax measurements, the distance to this system can be estimated as 66.2 light-years. It is receding from the Sun with a radial velocity of +23 km/s. This is a high proper motion star, traversing the celestial sphere at an angular rate of 0.333″·yr−1.

Gliese 809 is a red dwarf star in the constellation Cepheus, forming the primary component of a multi-star system. A visual magnitude of 8.55 makes it too faint to see with the naked eye. It is part of the Gliese Catalogue of Nearby Stars and is located about 23 light-years (ly) from the Solar System. Gliese 809 has about 70.5% the radius of the Sun and 61.4% of the Sun's mass. It has a metallicity of −0.06, which means that the abundance of elements other than hydrogen and helium is just 87.1% that of the Sun.

Gliese 180, is a small red dwarf star in the equatorial constellation of Eridanus. It is invisible to the naked eye with an apparent visual magnitude of 10.9. The star is located at a distance of 39 light years from the Sun based on parallax, and is drifting closer with a radial velocity of −14.6 km/s. It has a high proper motion, traversing the sky at the rate of 0.765 arcseconds per year.

GJ 3323 is a nearby single star located in the equatorial constellation Eridanus, about 0.4° to the northwest of the naked eye star Psi Eridani. It is invisible to the naked eye with an apparent visual magnitude 12.20. Parallax measurements give a distance estimate of 17.5 light-years from the Sun. It is drifting further away with a radial velocity of +42.3 km/s. Roughly 104,000 years ago, the star is believed to have come to within 7.34 ± 0.16 light-years of the Solar System.

Gliese 251, also known as HIP 33226 or HD 265866, is a star located about 18 light years away from the Solar System. Located in the constellation of Gemini, it is the nearest star in this constellation. It is located near the boundary with Auriga, 49 arcminutes away from the bright star Theta Geminorum; due to its apparent magnitude of +9.89 it cannot be observed with the naked eye. The closest star to Gliese 251 is QY Aurigae, which is located 3.5 light years away.

Gliese 588 is a nearby red dwarf star of spectral type M2.5, located in the constellation Lupus at 19.34 light-years from Earth. It emits a very stable light flux, with no detectable pulsations.

Gliese 514, also known as BD+11 2576 or HIP 65859, is a M-type main-sequence star, in the constellation Virgo 24.85 light-years away from the Sun. The proximity of Gliese 514 to the Sun was known exactly since 1988.

References

  1. 1 2 3 4 Perryman, M. A. C.; et al. (1997). "The Hipparcos Catalogue". Astronomy & Astrophysics. 323: L49–L52. Bibcode:1997A&A...323L..49P.
  2. 1 2 "NSV 15017 -- Flare Star". SIMBAD . Centre de Données astronomiques de Strasbourg. Archived from the original on 2019-06-05. Retrieved 2006-06-12.
  3. ↑ Houk, N.; Swift, C. (1982). "Michigan catalogue of two-dimensional spectral types for the HD Stars". Michigan Spectral Survey. 3. Bibcode:1982mcts.book.....H.
  4. 1 2 Cousins, A. W. J. (1973). "UBV Photometry of Some Southern Stars (Third List)". Monthly Notes of the Astronomical Society of Southern Africa. 32 (2): 43–48. Bibcode:1973MNSSA..32...43C.
  5. 1 2 "General Catalogue of Variable Stars NSV 15017". Centre de Données astronomiques de Strasbourg. Archived from the original on 2018-10-03. Retrieved 2009-12-14.
  6. ↑ Wilson, R. E. (1953). "General Catalogue of Stellar Radial Velocities". Carnegie Institution of Washington : 0. Bibcode:1953GCRV..C......0W.
  7. ↑ 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.
  8. ↑ Schmitt, JHMM; Liefke, C (April 2004). "NEXXUS: A comprehensive ROSAT survey of coronal X-ray emission among nearby solar-like stars". Astron. Astrophys. 417 (2): 651–65. arXiv: astro-ph/0308510 . Bibcode:2004A&A...417..651S. doi:10.1051/0004-6361:20030495. S2CID   17464039.
  9. 1 2 3 4 5 6 7 8 Maldonado, J.; Micela, G.; Baratella, M.; d'Orazi, V.; Affer, L.; Biazzo, K.; Lanza, A. F.; Maggio, A.; González Hernández, J. I.; Perger, M.; Pinamonti, M.; Scandariato, G.; Sozzetti, A.; Locci, D.; Di Maio, C.; Bignamini, A.; Claudi, R.; Molinari, E.; Rebolo, R.; Ribas, I.; Toledo-Padrón, B.; Covino, E.; Desidera, S.; Herrero, E.; Morales, J. C.; Suárez-Mascareño, A.; Pagano, I.; Petralia, A.; Piotto, G.; Poretti, E. (2020). "HADES RV programme with HARPS-N at TNG. XII. The abundance signature of M dwarf stars with planets". Astronomy and Astrophysics. 644: A68. arXiv: 2010.14867 . Bibcode:2020A&A...644A..68M. doi:10.1051/0004-6361/202039478. S2CID   225094682.
  10. ↑ Suárez Mascareño, A.; et al. (September 2015). "Rotation periods of late-type dwarf stars from time series high-resolution spectroscopy of chromospheric indicators". Monthly Notices of the Royal Astronomical Society. 452 (3): 2745–2756. arXiv: 1506.08039 . Bibcode:2015MNRAS.452.2745S. doi:10.1093/mnras/stv1441. S2CID   119181646.
  11. ↑ Schröder, C.; Reiners, Ansgar; Schmitt, Jürgen H. M. M. (January 2009). "Ca II HK emission in rapidly rotating stars. Evidence for an onset of the solar-type dynamo". Astronomy and Astrophysics. 493 (3): 1099–1107. Bibcode:2009A&A...493.1099S. doi: 10.1051/0004-6361:200810377 .
  12. ↑ Gould, B. (1885). "Star with large proper motion, in Sculptor". Astronomische Nachrichten . 111 (16): 255. Bibcode:1885AN....111..255G. doi:10.1002/asna.18851111612. Archived from the original on 2023-07-23. Retrieved 2019-07-04.
  13. ↑ Gliese, W. (1969). "Catalogue of Nearby Stars". Veröffentlichungen des Astronomischen Rechen-Instituts Heidelberg. 22: 1. Bibcode:1969VeARI..22....1G.
  14. ↑ Luyten, W. J. (1976). LHS (Luyten half-second) Catalogue. Minneapolis, Minnesota: University of Minnesota. Bibcode:1976lhsc.book.....L.
  15. ↑ M1.5: SIMBAD. M3: Gautier, Thomas N., III; et al. (2007). M3: Schmitt, J. H. M. M.; et al. (2004). M4: Eggen, Olin J. (1996) M4: Pasinetti-Fracassini, L. E.; et al. (2001).
  16. ↑ Pasinetti Fracassini, L. E.; Pastori, L.; Covino, S.; Pozzi, A. (February 2001). "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS) - Third edition - Comments and statistics". Astronomy and Astrophysics. 367 (2): 521–524. arXiv: astro-ph/0012289 . Bibcode:2001A&A...367..521P. doi:10.1051/0004-6361:20000451. S2CID   425754.Note: Search the VizieR catalogue II/224 Archived 2019-06-03 at the Wayback Machine for HD 225213.
  17. ↑ Schmitt, JHMM; Fleming, TA; Giampapa, MS (September 1995). "The X-ray view of the low-mass stars in the solar neighborhood". Astrophys. J. 450 (9): 392–400. Bibcode:1995ApJ...450..392S. doi: 10.1086/176149 .
  18. ↑ E. Lexen; R. Wehrse; J. Liebert; M. S. Bessell (January 2010). "The outer atmospheric layers of the early M dwarf Gliese 1". Astronomy and Astrophysics. 509: A101. Bibcode:2010A&A...509A.101L. doi: 10.1051/0004-6361/200912434 . hdl: 1885/36235 .
  19. ↑ Leinert, C.; Henry, T.; Glindemann, A.; McCarthy, D. W. Jr. (September 1997). "A search for companions to nearby southern M dwarfs with near-infrared speckle interferometry". Astronomy and Astrophysics. 325: 159–166. Bibcode:1997A&A...325..159L.
  20. ↑ Zechmeister, M.; Kürster, M.; Endl, M. (October 2009). "The M dwarf planet search programme at the ESO VLT + UVES. A search for terrestrial planets in the habitable zone of M dwarfs". Astronomy and Astrophysics. 505 (2): 859–871. arXiv: 0908.0944 . Bibcode:2009A&A...505..859Z. doi:10.1051/0004-6361/200912479. S2CID   16845441.
  21. ↑ Eggen, Olin J. (January 1996). "Distribution and Corrlation of Age, Abundance, and Motion of Lower Main Sequence Stars". Astronomical Journal. 111: 466–475. Bibcode:1996AJ....111..466E. doi: 10.1086/117797 .
  22. ↑ Allen, Christine; Santillan, Alfredo (October 1991). "An improved model of the galactic mass distribution for orbit computations". Revista Mexicana de Astronomía y Astrofísica. 22: 255–263. Bibcode:1991RMxAA..22..255A.
  23. ↑ Tetzlaff, N.; Neuhäuser, R.; Hohle, M. M. (January 2011). "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun". Monthly Notices of the Royal Astronomical Society . 410 (1): 190–200. arXiv: 1007.4883 . Bibcode:2011MNRAS.410..190T. doi:10.1111/j.1365-2966.2010.17434.x. S2CID   118629873.
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