From Wikipedia, the free encyclopedia
Rho Andromedae (ρ And, ρ Andromedae) is the Bayer designation for a star in the northern constellation of Andromeda . It has an apparent visual magnitude of +5.19,[ 2] Bortle Dark-Sky Scale , is bright enough to be seen with the naked eye from dark suburban skies. Based upon parallax measurements, this star is at a distance of approximately 158 light-years (48 parsecs ) from Earth .[ 1]
The stellar classification of this star is F5 III,[ 3] giant stage of its stellar evolution . However, some sources list a classification of F5 IV,[ 3] [ 6] subgiant stage. The interferometry -measured angular diameter of this star is 0.626 mas ,[ 6] radius of the Sun .[ 5] outer envelope is radiating around 20[ 6] effective temperature of 6,471 K,[ 7] [ 8] [ 4]
X-ray emissions were detected from this star during the EXOSAT mission.[ 9]
Naming
In Chinese , 天廄 Tiān Jiù Celestial Stable θ Andromedae and σ Andromedae . Consequently, the Chinese name for ρ Andromedae itself is 天廄二 Tiān Jiù èr Template:Lang-en .)[ 10]
References
^ a b c d e f van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics , 474 (2): 653–664, arXiv :0708.1752 Bibcode :2007A&A...474..653V , doi :10.1051/0004-6361:20078357 . ^ a b c d Breger, M. (March 1968), "UBV and narrow-band UVBY photometry of bright stars", Astronomical Journal , 73 : 84–85, Bibcode :1968AJ.....73...84B , doi :10.1086/110602 . ^ a b c d "* rho And -- Star" . SIMBAD Centre de données astronomiques de Strasbourg . Retrieved 2012-06-24 .{{cite web }}: CS1 maint: postscript (link )^ a b c d Nordström, B.; et al. (May 2004), "The Geneva-Copenhagen survey of the Solar neighbourhood. Ages, metallicities, and kinematic properties of ˜14 000 F and G dwarfs", Astronomy and Astrophysics , 418 : 989–1019, arXiv :astro-ph/0405198 Bibcode :2004A&A...418..989N , doi :10.1051/0004-6361:20035959 . ^ a b Lang, Kenneth R. (2006), Astrophysical formulae Birkhäuser , ISBN 3-540-29692-1 * ) is given by:
2
⋅
R
∗
=
(
48.5
⋅
0.626
⋅
10
−
3
)
AU
0.0046491
AU
/
R
⨀
≈
6.5
⋅
R
⨀
{\displaystyle {\begin{aligned}2\cdot R_{*}&={\frac {(48.5\cdot 0.626\cdot 10^{-3})\ {\text{AU}}}{0.0046491\ {\text{AU}}/R_{\bigodot }}}\\&\approx 6.5\cdot R_{\bigodot }\end{aligned}}}
^ a b c d van Belle, G. T.; et al. (May 2008), "The Palomar Testbed Interferometer Calibrator Catalog", The Astrophysical Journal Supplement Series , 176 (1): 276–292, arXiv :0711.4194 Bibcode :2008ApJS..176..276V , doi :10.1086/526548 . {{citation }}: CS1 maint: multiple names: authors list (link )^ a b c d e Balachandran, Suchitra (May 1, 1990). "Lithium depletion and rotation in main-sequence stars". Astrophysical Journal, Part 1 . 354 : 310–332. Bibcode :1990ApJ...354..310B . doi :10.1086/168691 . {{cite journal }}: CS1 maint: postscript (link )^ "The Colour of Stars" , Australia Telescope, Outreach and Education , Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, retrieved 2012-01-16 .^ Gondoin, P.; Mangeney, A.; Praderie, F. (March 1987), "Solar-type giants - New X-ray detections from EXOSAT observations", Astronomy and Astrophysics , 174 (1–2): 187–196, Bibcode :1987A&A...174..187G . ^ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 5 月 18 日
External links
