| 词条 | 50 Persei |
| 释义 |
| name = 50 Persei }}{{Starbox observe | epoch = J2000.0 | constell = Perseus | ra = {{RA|04|08|36.61660}} | dec = {{DEC|+38|02|23.0488}} | appmag_v = 5.52[3] }}{{Starbox character | class = F7 V[4] | b-v = +0.54[3] | u-b = +0.00[3] | variable = RS CVn and BY Dra }}{{Starbox astrometry | radial_v = +26.2[7] | prop_mo_ra = +164.10 | prop_mo_dec = −202.60 | parallax = 47.63 | p_error = 0.26 | parallax_footnote = | absmag_v = 3.87[11] }}{{Starbox detail | mass = 1.16[12] | radius = | luminosity = | gravity = 4.35[12] | temperature = 6,147[12] | metal_fe = −0.11[12] | rotational_velocity = 20.81[16] | age_gyr = 0.60[17] }}{{Starbox catalog | names = 50 Per, BD+37° 882, FK5 2297, GJ 9145, HD 25998, HIP 19335, HR 1278, SAO 57006.[18] }}{{Starbox reference |Simbad=50+Per }}{{Starbox end}}50 Persei is a star in the constellation Perseus. Its apparent magnitude is 5.52,[3] which is bright enough to be seen with the naked eye. Located around {{convert|21.00|pc|ly}} distant, it is a White main-sequence star of spectral type F7V,[4] a star that is currently fusing its core hydrogen. In 1998 the star was named a candidate Gamma Doradus variable with a period of 3.05 days,[11] which would means it displays variations in luminosity due to non-radial pulsations in the photosphere. Subsequently, it was classified as a RS Canum Venaticorum and BY Draconis variable by an automated program.[22] This is probably a binary system with an unseen companion. It is physically associated with the likely binary system HIP 19255, with the two pairs orbiting each other over a time scale of around a million years. The components of HIP 19255 have an angular separation of 3.87″ and the two components orbit each other every 590 years. 50 Persei may share a gravitational association with Capella, even though the two are separated by nearly 15° − equivalent to a distance of {{Convert|5.9|pc|ly|abbr=on|lk=off|order=flip}}.[23] 50 Persei is emitting an infrared excess at a wavelength of 70 μm, suggesting the presence of a circumstellar debris disk. The disk has a temperature of {{Val|96|5|u=K}}.[17] References1. ^1 2 {{citation | display-authors=1 | last1=Maldonado | first1=J. | last2=Martínez-Arnáiz | first2=R. 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F. | title=New Debris Disks around Nearby Main-Sequence Stars: Impact on the Direct Detection of Planets | journal=The Astrophysical Journal | volume=652 | issue=2 | pages=1674–1693 | date=December 2006 | doi=10.1086/508449 | bibcode=2006ApJ...652.1674B | arxiv=astro-ph/0611682 | postscript=. }} 9. ^1 2 3 4 {{citation | last1=Mermilliod | first1=J.-C. | title=Compilation of Eggen's UBV data, transformed to UBV (unpublished) | work=SIMBAD Astronomical Database | date=1986 | bibcode=1986EgUBV........0M | postscript=. }} 10. ^1 {{cite simbad | title=* 50 Per | accessdate=2016-07-22 | postscript=. }} }}{{Stars of Perseus}} 11 : Perseus (constellation)|Flamsteed objects|F-type main-sequence stars|Objects with variable star designations|RS Canum Venaticorum variables|Hipparcos objects|HR objects|Henry Draper Catalogue objects|Gliese and GJ objects|BY Draconis variables|Durchmusterung objects |
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