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Gliese 328

Coordinates:Sky map08h 55m 07.6219s, +01° 32′ 47.4165″
From Wikipedia, the free encyclopedia
Gliese 328
Observation data
Epoch J2000      Equinox J2000
ConstellationHydra
Right ascension08h 55m 07.62173s[1]
Declination+01° 32′ 47.4151″[1]
Apparent magnitude (V)9.997[2]
Characteristics
Evolutionary stagemain-sequence star
Spectral typeM0V[2]
B−Vcolor index1.30[2]
Astrometry
Radial velocity (Rv)−3.731±0.0015[3] km/s
Proper motion (μ)RA: 44.944mas/yr[1]
Dec.: −1045.876mas/yr[1]
Parallax (π)48.7404±0.0184 mas[1]
Distance66.92 ± 0.03 ly
(20.517 ± 0.008 pc)
Details[2]
Mass0.65±0.08 M
Radius0.63±0.07 R
Luminosity0.08 L
Surface gravity (log g)4.64±0.07 cgs
Temperature3897±71 K
Metallicity [Fe/H]−0.06±0.09 dex
Rotation33.6 days[4]
Other designations
BD+02 2098,GJ 328,HIP 43790,Ross 623,TYC 213-177-1,2MASS J08550761+0132472[3]
Database references
SIMBADdata

Gliese 328, also known as BD+02 2098, is ared dwarf star located 66.9light-years (20.5parsecs) away in the constellationHydra. Its surface temperature is 3989K. Gliese 328 is depleted in heavy elements compared to theSun, with ametallicity Fe/H index of −0.13.[5] The age of the star is unknown. Gliese 328 exhibits an activity cycle similar to that of theSun, with a period around 2000d.[4]

Multiplicity surveys did not detect any stellar companions as of 2016.[6]

Planetary system

[edit]

In 2013, onesuperjovian planet, named Gliese 328 b, was discovered on a wide, eccentric orbit by theradial velocity method.[7] The known planetary orbit is wide enough to not disrupt orbits of other bodies in the habitable zone of the star.[8] In 2023, a second, Neptune-mass planet was discovered orbiting closer to the star.[2]

The Gliese 328 planetary system[2]
Companion
(in order from star)
MassSemimajor axis
(AU)
Orbital period
(days)
EccentricityInclinationRadius
c≥21.4+3.4
−3.2
 M🜨
0.657+0.026
−0.028
241.8+1.3
−1.7
b≥2.51±0.23 MJ4.11+0.16
−0.18
3771±170.227±0.015

References

[edit]
  1. ^abcdVallenari, 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 atVizieR.
  2. ^abcdefPinamonti, M.; Barbato, D.; et al. (June 2023). "The GAPS programme at TNG. XLVI. Deep search for low-mass planets in late-dwarf systems hosting cold Jupiters".Astronomy & Astrophysics.677.arXiv:2306.04419.Bibcode:2023A&A...677A.122P.doi:10.1051/0004-6361/202346476.
  3. ^ab"BD+02 2098".SIMBAD.Centre de données astronomiques de Strasbourg. Retrieved2021-02-03.
  4. ^abKüker, M.; Rüdiger, G.; Olah, K.; Strassmeier, K. G. (2019), "Cycle period, differential rotation and meridional flow for early M dwarf stars",Astronomy & Astrophysics,622: A40,arXiv:1804.02925,Bibcode:2019A&A...622A..40K,doi:10.1051/0004-6361/201833173,S2CID 118842388
  5. ^Wallerstein, George; Woolf, Vincent M. (2020), "The M dwarf problem: Fe and Ti abundances in a volume-limited sample of M dwarf stars",Monthly Notices of the Royal Astronomical Society,494 (2):2718–2726,arXiv:2003.11447,Bibcode:2020MNRAS.494.2718W,doi:10.1093/mnras/staa878,S2CID 214641078
  6. ^Ginski, C.; Mugrauer, M.; Seeliger, M.; Buder, S.; Errmann, R.; Avenhaus, H.; Mouillet, D.; Maire, A.-L.; Raetz, S. (2016), "A lucky imaging multiplicity study of exoplanet host stars II",Monthly Notices of the Royal Astronomical Society,457 (2):2173–2191,arXiv:1601.01524,Bibcode:2016MNRAS.457.2173G,doi:10.1093/mnras/stw049,S2CID 53626523
  7. ^Robertson, Paul; Endl, Michael; Cochran, William D.; MacQueen, Phillip J.; Boss, Alan P. (2013), "Secretly Eccentric: The Giant Planet and Activity Cycle of GJ 328",The Astrophysical Journal,774 (2): 147,arXiv:1307.7640,Bibcode:2013ApJ...774..147R,doi:10.1088/0004-637X/774/2/147,S2CID 118514735
  8. ^Kokaia, Giorgi; Davies, Melvyn B.; Mustill, Alexander J. (2020), "Resilient habitability of nearby exoplanet systems",Monthly Notices of the Royal Astronomical Society,492 (1):352–368,arXiv:1910.07573,Bibcode:2020MNRAS.492..352K,doi:10.1093/mnras/stz3408,S2CID 204743669


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