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GRW +70 8247

From Wikipedia, the free encyclopedia
(Redirected fromGJ 742)
Star in the constellation Draco
GRW +70 8247
Observation data
EpochJ2000.0      EquinoxJ2000.0 (ICRS)
ConstellationDraco
Right ascension19h 00m 10.2534s[1]
Declination+70° 39′ 51.418″[1]
Apparent magnitude (V)13.19[2]
Characteristics
Spectral typeDAP4.5[3]
U−Bcolor index-0.85[4]
B−Vcolor index+0.05[4]
Astrometry
Proper motion (μ)RA: +85.774[1]mas/yr
Dec.: +505.050[1]mas/yr
Parallax (π)77.6525±0.0317 mas[1]
Distance42.00 ± 0.02 ly
(12.878 ± 0.005 pc)
Details[5]
Mass1.029 M
Radius5,960[a] km
Luminosity0.013182 L
Surface gravity (log g)8.67 cgs
Temperature12540±143 K
Age(as white dwarf) 1.138 Gyr
Other designations
GJ 742,AC +70 8247,G 260-15, LFT 1446,LHS 3424, LTT 15585,Grw+70 8247, WD 1900+705[2][6]
Database references
SIMBADdata
ARICNSdata

GRW +70 8247 is awhite dwarf star located 42 light-years fromEarth[1] in theconstellationDraco. With amagnitude of about 13 it is visible only through a largetelescope.

Properties

[edit]

Although photographed in the 19th century as part of theCarte du Ciel project, the star was not determined to be a white dwarf untilG. P. Kuiper observed it in 1934.[7] This makes it the fifth or sixth white dwarf discovered.[b] At first, itsspectrum was thought to be almost featureless,[7] but later observation showed it to have unusual broad, shallowabsorption bands.[11][12] In 1970, when light that it emitted was observed to becircularly polarized, it became the first white dwarf known to have amagnetic field.[13][14] In the 1980s, it was realized that the unusual absorption bands could be explained ashydrogen absorption lines shifted by theZeeman effect.[6][15][16]

Notes

[edit]
  1. ^ Applying theStefan–Boltzmann law with a nominalsolareffective temperature of 5,772 K:
    (5,77211,880)4102.88=0.00857 R{\displaystyle {\sqrt {{\biggl (}{\frac {5,772}{11,880}}{\biggr )}^{4}\cdot 10^{-2.88}}}=0.00857\ R_{\odot }}.
  2. ^The star EGGR 37 was suspected to be a white dwarf by April 1934,[8] but this was not confirmed until 1938.[9][10]

References

[edit]
  1. ^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.
  2. ^ab"LAWD 73".SIMBAD.Centre de données astronomiques de Strasbourg. RetrievedNovember 5, 2007.
  3. ^Wesemael, F.; Greenstein, J. L.; Liebert, James; Lamontagne, R.; Fontaine, G.; Bergeron, P.; Glaspey, J. W. (1993)."An atlas of optical spectra of white-dwarf stars".Publications of the Astronomical Society of the Pacific.105: 761.Bibcode:1993PASP..105..761W.doi:10.1086/133228.S2CID 122605705.
  4. ^abMermilliod, J.-C. (1986)."Compilation of Eggen's UBV data, transformed to UBV (unpublished)".Catalogue of Eggen's UBV Data.Bibcode:1986EgUBV........0M.
  5. ^"GJ 742".Montreal White Dwarf Database. Retrieved2024-05-30.
  6. ^abJesse L. Greenstein, Ronald J. W. Henry, and R. F. O'Connell (February 15, 1985)."Further identifications of hydrogen in Grw +70°8247".Astrophysical Journal.289:L25–L29.Bibcode:1985ApJ...289L..25G.doi:10.1086/184427.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  7. ^abG. P. Kuiper (October 1934)."Two New White Dwarfs of Large Parallax".Publications of the Astronomical Society of the Pacific.46 (273):287–290.Bibcode:1934PASP...46..287K.doi:10.1086/124496.S2CID 123421818.
  8. ^P. J. van Rhijn and J. J. Raimond (April 1934)."Some new members of the Hyades cluster".Monthly Notices of the Royal Astronomical Society.94 (6):508–518, at p. 517.Bibcode:1934MNRAS..94..508V.doi:10.1093/mnras/94.6.508.
  9. ^Jöran M. Ramberg (May 1938)."Zwei weiße Zwerge unter den physischen Hyadenmigliedern".Astronomische Nachrichten (in German).265 (6–7):111–112.Bibcode:1938AN....265..111R.doi:10.1002/asna.19382650609.
  10. ^See alsoGerard P. Kuiper (August 1941)."List of Known White Dwarfs".Publications of the Astronomical Society of the Pacific.53 (314):248–252.Bibcode:1941PASP...53..248K.doi:10.1086/125335.S2CID 123040354.
  11. ^Walter S. Adams and Frederick H. Seahes (1938)."Annual Report of the Director of the Mount Wilson Observatory (1937-1938)".Mount Wilson Observatory Annual Report.10: 28.Bibcode:1938MWOAR..10....1A.
  12. ^Jesse L. Greenstein and Mildred S. Matthews (July 1957)."Studies of the White Dwarfs. I. Broad Features in White Dwarf Spectra".Astrophysical Journal.126:14–18.Bibcode:1957ApJ...126...14G.doi:10.1086/146364.
  13. ^James C. Kemp, John B. Swedlund, J. D. Landstreet, and J. R. P. Angel (August 1970)."Discovery of Circularly Polarized Light from a White Dwarf".Astrophysical Journal.161:L77–L79.Bibcode:1970ApJ...161L..77K.doi:10.1086/180574.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  14. ^Angel, J.R.P.; Landstreet, J.D.; Oke, J.B. (1972)."The Spectral Dependence of Circular Polarization in Grw+70°8247".Astrophysical Journal.171:L11–L15.Bibcode:1972ApJ...171L..11A.doi:10.1086/180857.
  15. ^J. R. P. Angel, James Liebert, and H. S. Stockman (May 1, 1985)."The optical spectrum of hydrogen at 160-350 million gauss in the white dwarf Grw +70°8247".Astrophysical Journal.292:260–266.Bibcode:1985ApJ...292..260A.doi:10.1086/163156.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  16. ^D. T. Wickramasinghe and Lilia Ferrario (April 1, 1988)."A centered dipole model for the high field magnetic white dwarf GRW +70°8247".Astrophysical Journal.327:222–233.Bibcode:1988ApJ...327..222W.doi:10.1086/166184.


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