释义 |
- References
{{Starbox begin | name = W Corvi }}{{Starbox observe | epoch = J2000.0 | equino = J2000.0 | constell = Corvus | ra = {{RA|12|07|34.360}}[1] | dec = {{DEC|-13|08|59.02}}[1] | appmag_v = 11.16 - 12.5 }}{{Starbox character | type = Beta Lyrae variable | class = G- | b-v = }}{{Starbox astrometry | radial_v = | prop_mo_ra = -18.8 ± 2.1 | prop_mo_dec = 18.2 ± 2.1 | parallax = | p_error = | parallax_footnote = | dist_pc = | absmag_v ={{Starbox detail | source = | mass = | radius = | gravity = | luminosity = | luminosity_bolometric = | luminosity_visual = | temperature = | metal = | rotation = | rotational_velocity = | age = | age_gyr = }}{{Starbox catalog | names = W Corvi, BD−12° 3565 }}{{Starbox reference |Simbad=W+Crv }}{{Starbox end}}W Corvi is an eclipsing binary star system in the constellation Corvus, ranging from apparent magnitude 11.16 to 12.5 over 9 hours.[ Its period has increased by 1/4 second over a century. It is an unusual system in that its two stars are very close to each other yet have different surface temperatures and hence thermal transfer is not taking place as expected.[5]]References1. ^1 {{cite web|url=http://simbad.u-strasbg.fr/simbad/sim-id?Ident=W+Crv&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id |title=W Crv -- Eclipsing binary of beta Lyr type (semi-detached) |accessdate=21 July 2015}} 2. ^1 {{cite journal|title=Changes in the Period and Light Curve of W Corvi| author=Odell, Andrew P. |journal=Monthly Notices of the Royal Astronomical Society | volume=282 |issue=2 |pages=373–83 |date=1996 |bibcode=1996MNRAS.282..373O |doi=10.1093/mnras/282.2.373}}
[2] }}{{Stars of Corvus}}{{star-system-stub}} 2 : Corvus (constellation)|Beta Lyrae variables |