GJ 1005

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GJ 1005
Observation data
Epoch J2000        Equinox J2000
Constellation Cetus
Right ascension 00h 15m 28.11090s [1]
Declination −16° 08′ 01.6303″ [1]
Apparent magnitude  (V)11.483 [2]
Characteristics
Spectral type M3.5V [3]
Astrometry
Radial velocity (Rv)-26.43 ± 0.1 [4]  km/s
Proper motion (μ)RA: 731.83 [1]   mas/yr
Dec.: -607.73 [1]   mas/yr
Parallax (π)166.6 ± 0.3  mas [3]
Distance 19.58 ± 0.04  ly
(6.00 ± 0.01  pc)
Absolute magnitude  (MV)12.70 ± 0.01 / 15.12 ± 0.09 [3]
Orbit [3]
Period (P)4.55726+0.00075
−0.00074 y. [5]
Semi-major axis (a)0.3037 ± 0.0005″
Eccentricity (e)0.36136+0.00097
−0.00098 [5]
Inclination (i)143.93+0.25
−0.24 [5] °
Longitude of the node (Ω)62.8 ± 0.4°
Periastron epoch (T) JD 2449850.4 ± 0.8
Argument of periastron (ω)
(secondary)		166.6 ± 0.5°
Details [3]
GJ 1005 A
Mass 0.179 ± 0.002  M☉
Temperature 3341±224 [6]   K
Metallicity [Fe/H]-0.41 [5]   dex
GJ 1005 B
Mass 0.112 ± 0.001  M☉
Other designations
Gaia DR2  2368293487260807040, HIP  1242, G 158-50, G 266-76, LHS  1047, LP  764-87, LTT  114, 2MASS J00152799-1608008
Database references
SIMBAD data
ARICNS A
B
Cetus constellation map.svg
Red pog.png
GJ 1005
Location of GJ 1005 in the constellation Cetus

GJ 1005 is a system of two red dwarfs, located in constellation Cetus at 19.6 light-years from Earth. [7] The primary star is a M4V class star while the secondary is a class M7V.[ citation needed ]

The system was observed with the Hubble Space Telescope in the 1990s with its Fine Guidance Sensor. [7] This data helped determine the mass of each of the components of L722-22/ LHS 1047 / GJ 1005. [7]

Related Research Articles

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<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 first 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.

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.

Pi Mensae, also known as HD 39091, is a yellow dwarf star in the constellation of Mensa. This star has a high proper motion. The apparent magnitude is 5.67, which can be visible to the naked eye in exceptionally dark, clear skies. It is nearly 60 light-years away. The star is slightly larger than the Sun in terms of mass, size, luminosity, temperature and metallicity, and is about 730 million years younger. It hosts three known planets.

Gliese 849, or GJ 849, is a small, solitary star in the equatorial constellation of Aquarius. It has a reddish hue and is invisible to the naked eye with an apparent visual magnitude of 10.41. The distance to this star is 28.7 light years based on parallax, but it is drifting closer to the Sun with a radial velocity of −15.3 km/s. It has a pair of confirmed gas giant companions.

<span class="mw-page-title-main">Gliese 22</span> Star in the constellation Cassiopeia

Gliese 22, also catalogued V547 Cassiopeiae or ADS 440, is a hierarchical star system approximately 33 light-years away in the constellation of Cassiopeia. The system consists of pair of red dwarf stars, Gliese 22A and Gliese 22C, orbited by a third red dwarf Gliese 22B in an outer orbit of about 223 years.

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.

<span class="mw-page-title-main">Gliese 180</span> Star in the constellation Eridanus

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.

Gliese 54 is a star near the Solar System located at 25.7 light years away. It is located in the constellation of Tucana, close to the edge, almost in the neighboring Hydrus. It is below the threshold brightness to be observable eye with an apparent magnitude of +9.80,.

<span class="mw-page-title-main">51 Eridani</span> F-type main sequence star in the constellation Eridanus

51 Eridani is a star in the constellation Eridanus. It has an apparent magnitude of 5.22, meaning it is just visible to the unaided eye in suburban and rural skies. The primary star's absolute magnitude is 2.87. There is also a binary star named GJ 3305 which shares the same proper motion through space with it, making it overall a triple star system.

<span class="mw-page-title-main">HD 203030</span> K-type main sequence star in the constellation Vulpecula

HD 203030 is a single, yellow-orange hued star with a sub-stellar companion in the northern constellation of Vulpecula. The designation HD 203030 is from the Henry Draper Catalogue, which is based on spectral classifications made between 1911 and 1915 by Annie Jump Cannon and her co-workers, and was published between 1918 and 1924. This star is invisible to the naked eye, having an apparent visual magnitude of 8.45. It is located at a distance of 128 light years from the Sun based on parallax, and is drifting closer with a radial velocity of −17 km/s.

<span class="mw-page-title-main">V1005 Orionis</span> Young flame star in the constellation of Orion

V1005 Orionis is a young flare star in the equatorial constellation of Orion. It has the identifier GJ 182 in the Gliese–Jahreiß catalogue; V1005 Ori is its variable star designation. This star is too faint to be visible to the naked eye, having a mean apparent visual magnitude of 10.1. It is located at a distance of 79.6 light years from the Sun and is drifting further away with a radial velocity of 19.2 km/s. The star is a possible member of the IC 2391 supercluster.

<span class="mw-page-title-main">14 Trianguli</span> Star in the constellation Triangulum

14 Trianguli, also known as HD 15656, is a spectroscopic binary located in the northern constellation Triangulum. It has an apparent magnitude of 5.14, making it faintly visible to the naked eye in ideal conditions. Gaia DR3 parallax measurements place the system 433 light years away, and it is currently approaching the Solar System with a heliocentric radial velocity of −37 km/s. At its current distance, 14 Tri's brightness is diminished by 0.21 magnitude due to interstellar dust. It has an absolute magnitude of −0.46.

HD 10800, also known as HR 512 or Gliese 67.1, is a triple star located in the southern circumpolar constellation Octans. It has a combined apparent magnitude of 5.87, allowing it to be faintly seen with the naked eye. The system is relatively close at a distance of 88.1 light years but is drifting closer with a heliocentric radial velocity −1.1 km/s.

HR 8526, also known as HD 212168, is the primary of a triple star located in the southern circumpolar constellation Octans. The star and its companion have apparent magnitudes of 6.12 and 9.36 respectively.The system is located relatively close at a distance of 76 light years based on Gaia DR3 parallax measurements, but is receding with a heliocentric radial velocity of 15 km/s.

References

  1. 1 2 3 4 van Leeuwen, F.; et al. (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.
  2. ↑ Koen, C.; Kilkenny, D.; van Wyk, F.; Marang, F. (2010). "UBV(RI)C JHK observations of Hipparcos-selected nearby stars". Monthly Notices of the Royal Astronomical Society. 403 (4): 1949–1968. Bibcode:2010MNRAS.403.1949K. doi: 10.1111/j.1365-2966.2009.16182.x .
  3. 1 2 3 4 5 Benedict, G. F.; Henry, T. J.; Franz, O. G.; McArthur, B. E.; Wasserman, L. H.; Jao, Wei-Chun; Cargile, P. A.; Dieterich, S. B.; Bradley, A. J.; Nelan, E. P.; Whipple, A. L. (2016). "The Solar Neighborhood. XXXVII. The Mass–Luminosity Relation for Main-Sequence M Dwarfs". The Astronomical Journal. 152 (5): 141. arXiv: 1608.04775 . Bibcode:2016AJ....152..141B. doi:10.3847/0004-6256/152/5/141. S2CID   54029447.
  4. ↑ Nidever, David L.; et al. (2013). "Radial Velocities for 889 Late-Type Stars". The Astrophysical Journal Supplement Series. 141 (2): 503–522. arXiv: astro-ph/0112477 . Bibcode:2002ApJS..141..503N. doi:10.1086/340570. S2CID   51814894.
  5. 1 2 3 4 Mann, Andrew W.; Dupuy, Trent; Kraus, Adam L.; Gaidos, Eric; Ansdell, Megan; Ireland, Michael; Rizzuto, Aaron C.; Hung, Chao-Ling; Dittmann, Jason; Factor, Samuel; Feiden, Gregory; Martinez, Raquel A.; Ruíz-Rodríguez, Dary; Chia Thao, Pa (2019), "How to Constrain Your M Dwarf. II. The Mass–Luminosity–Metallicity Relation from 0.075 to 0.70 Solar Masses", The Astrophysical Journal, 871 (1): 63, arXiv: 1811.06938 , Bibcode:2019ApJ...871...63M, doi:10.3847/1538-4357/aaf3bc, S2CID   119372932
  6. ↑ Costa-Almeida, Ellen; De Mello, Gustavo F Porto; Giribaldi, Riano E.; Lorenzo-Oliveira, Diego; Ubaldo-Melo, Maria L. (2021), "M dwarf spectral indices at moderate resolution: Accurate Teff and [Fe/H] for 178 southern stars", Monthly Notices of the Royal Astronomical Society, 508 (4): 5148–5162, arXiv: 2110.01658 , doi:10.1093/mnras/stab2831
  7. 1 2 3 Hershey, John L.; Taff, L. G. (1998-01-01). "Hubble Space Telescope Fine Guidance Sensor Astrometry of the Low-Mass Binary L722-22". The Astronomical Journal. 116 (3): 1440. Bibcode:1998AJ....116.1440H. doi: 10.1086/300516 . ISSN   1538-3881.
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