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HD 221246

From Wikipedia, the free encyclopedia
Star in the open cluster NGC 7686
HD 221246
Observation data
Epoch J2000      Equinox J2000
ConstellationAndromeda[1]
Right ascension23h 30m 07.4133s[2]
Declination+49° 07′ 59.323″[2]
Apparent magnitude (V)6.17[3]
Characteristics
Spectral typeK3III[4]
U−Bcolor index1.71[3]
B−Vcolor index1.46[3]
Astrometry
Radial velocity (Rv)−8.41±0.15[5] km/s
Proper motion (μ)RA: 28.741±0.100[2]mas/yr
Dec.: 3.180±0.087[2]mas/yr
Parallax (π)3.2290±0.0642 mas[2]
Distance1,010 ± 20 ly
(310 ± 6 pc)
Absolute magnitude (MV)−0.97[1]
Details
Mass1.4[6] M
Radius44[7] R
Luminosity690[6] L
Surface gravity (log g)1.20[6] cgs
Temperature4,285[6] K
Metallicity[Fe/H]−0.24±0.10[8] dex
Other designations
BD+48°4070,FK5 3882,HD 221246,HIP 115996,HR 8925,NGC 7686 1,SAO 53088
Database references
SIMBADdata

HD 221246 orNGC 7686 1 is a star inopen clusterNGC 7686, and it belongs to the northernconstellation ofAndromeda. With anapparent visual magnitude of 6.17,[3] it can be viewed by the naked eye only under very favourable conditions. It has aspectral classification of K3III, meaning it is an evolved orangegiant star.[4]Parallax measurements place this star about 1,000light years away from the Solar System.[2]

References

[edit]
  1. ^abAnderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation".Astronomy Letters.38 (5): 331.arXiv:1108.4971.Bibcode:2012AstL...38..331A.doi:10.1134/S1063773712050015. XHIP record for this object atVizieR.
  2. ^abcdefBrown, A. G. A.; et al. (Gaia collaboration) (August 2018)."Gaia Data Release 2: Summary of the contents and survey properties".Astronomy & Astrophysics.616. A1.arXiv:1804.09365.Bibcode:2018A&A...616A...1G.doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source atVizieR.
  3. ^abcdJohnson, H. L.; et al. (1966), "UBVRIJKL photometry of the bright stars",Communications of the Lunar and Planetary Laboratory,4 (99): 99,Bibcode:1966CoLPL...4...99J
  4. ^abShenavrin, V. I.; et al. (2011). "Search for and study of hot circumstellar dust envelopes".Astronomy Reports.55 (1):31–81.Bibcode:2011ARep...55...31S.doi:10.1134/S1063772911010070.S2CID 122700080.
  5. ^Famaey, B.; Jorissen, A.; Luri, X.; Mayor, M.; Udry, S.; Dejonghe, H.; Turon, C. (2005). "Local kinematics of K and M giants from CORAVEL/Hipparcos/Tycho-2 data. Revisiting the concept of superclusters".Astronomy and Astrophysics.430:165–186.arXiv:astro-ph/0409579.Bibcode:2005A&A...430..165F.doi:10.1051/0004-6361:20041272.S2CID 17804304.
  6. ^abcdFouesneau, M.; Andrae, R.; Dharmawardena, T.; Rybizki, J.; Bailer-Jones, C. A. L.; Demleitner, M. (2022). "Astrophysical parameters from Gaia DR2, 2MASS, and AllWISE".Astronomy and Astrophysics.662: A125.arXiv:2201.03252.Bibcode:2022A&A...662A.125F.doi:10.1051/0004-6361/202141828.
  7. ^Stassun, Keivan G.; et al. (2019)."The Revised TESS Input Catalog and Candidate Target List".The Astronomical Journal.158 (4): 138.arXiv:1905.10694.Bibcode:2019AJ....158..138S.doi:10.3847/1538-3881/ab3467.
  8. ^Röck, B.; Vazdekis, A.; Peletier, R. F.; Knapen, J. H.; Falcón-Barroso, J. (2015)."Stellar population synthesis models between 2.5 and 5 μm based on the empirical IRTF stellar library".Monthly Notices of the Royal Astronomical Society.449 (3): 2853.arXiv:1505.01837.Bibcode:2015MNRAS.449.2853R.doi:10.1093/mnras/stv503.

External links

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