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GJ 1005

Coordinates:Sky map00h 15m 28.11090s, −16° 08′ 01.6303″
From Wikipedia, the free encyclopedia
Star system in the constellation Cetus
GJ 1005
Observation data
EpochJ2000      EquinoxJ2000
ConstellationCetus
Right ascension00h 15m 28.11090s[1]
Declination−16° 08′ 01.6303″[1]
Apparent magnitude (V)11.483[2]
Characteristics
Spectral typeM3.5V[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]
Distance19.58 ± 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°
Periastronepoch (T)JD 2449850.4 ± 0.8
Argument of periastron (ω)
(secondary)
166.6 ± 0.5°
Details[3]
GJ 1005 A
Mass0.179 ± 0.002 M
Temperature3341±224[6] K
Metallicity [Fe/H]-0.41[5] dex
GJ 1005 B
Mass0.112 ± 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
SIMBADdata
ARICNSA
B
GJ 1005 is located in the constellation Cetus.
GJ 1005 is located in the constellation Cetus.
GJ 1005
Location of GJ 1005 in the constellationCetus

GJ 1005 is a system of twored dwarfs, located inconstellationCetus at 19.6light-years fromEarth.[7] The primary star is a M4Vclass star while the secondary is a class M7V.[citation needed]

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

References

[edit]
  1. ^abcdvan 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. ^abcdeBenedict, 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. ^abcdMann, 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. ^abcHershey, 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.
Primary membertype
Celestial objects by systems. Secondary members are listed in small print.
    0–10ly
Main-sequence
stars
A-type
G-type
M-type
(red dwarfs)
Brown dwarfs
L-type
  • Luhman 16 (6.5029±0.0011 ly)
  • T-type brown dwarf B
Sub-brown dwarfs
androgue planets
Y-type
10–15ly
Subgiant stars
F-type
Main-sequence
stars
G-type
  • Tau Ceti (11.9118±0.0074 ly)
  • 4 (8?) planets: (b), (c), (d), e, f, g, h, (i)
K-type
M-type
(red dwarfs)
Degenerate
stars
White dwarfs
Brown dwarfs
T-type
15–20ly    
Subgiant stars
G-type
Main-sequence
stars
A-type
G-type
K-type
M-type
(red dwarfs)
Degenerate
stars
White dwarfs
Brown dwarfs
L-type
T-type
Y-type
Sub-brown dwarfs
androgue planets
Y-type
Italic are systems without knowntrigonometric parallax.
Stars
Bayer
Flamsteed
Variable
HR
HD
Other
Exoplanets
Nebulae
Galaxies
Messier
NGC
Other
Galaxy clusters
Astronomical events
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