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OU Andromedae

From Wikipedia, the free encyclopedia
Rotationally variable star in the constellation Andromeda
OU Andromedae

The light curve of anX-ray flare observed in 2001 by theChandra X-ray Observatory is shown. This flare is believed to have been produced by acoronal mass ejection. (Adapted from Argiroffiet al., 2019[1])
Observation data
Epoch J2000      Equinox J2000
ConstellationAndromeda
Right ascension23h 49m 40.9595s[2]
Declination+36° 25′ 31.013″[2]
Apparent magnitude (V)5.87 - 5.94[3]
Characteristics
Evolutionary stagesubgiant[4]
Spectral typeG1 IIIe[5]
Apparent magnitude (G)5.638[2]
Apparent magnitude (J)4.723[6]
Apparent magnitude (H)4.208[6]
Apparent magnitude (K)4.097[6]
B−Vcolor index0.79[5]
Variable typeFK Com[3]
Astrometry
Radial velocity (Rv)−1.79±0.14[2] km/s
Proper motion (μ)RA: −0.634±0.046[2]mas/yr
Dec.: −47.740±0.028[2]mas/yr
Parallax (π)7.2647±0.0411 mas[2]
Distance449 ± 3 ly
(137.7 ± 0.8 pc)
Details[4]
Mass2.85 M
Radius9.46 R
Luminosity71.2 L
Surface gravity (log g)2.8 cgs
Temperature5,360 K
Metallicity[Fe/H]−0.07 dex
Rotation24.3 days
Rotational velocity (v sin i)21.5 km/s
Age346[2] Myr
Other designations
2MASS J23494097+3625309,FK5 3914,HIP 117503,SAO 73535,BD+35°5110,HR 9024,HD 223460,PPM 89159
Database references
SIMBADdata

OU Andromedae (alsoHR 9024) is a rotationallyvariable star in theconstellationAndromeda. Varying between magnitudes 5.87 and 5.94, it has been classified as anFK Comae Berenices variable, but the classification is still uncertain. It has aspectral classification of G1IIIe, meaning that it is agiant star that showsemission lines in its spectrum.[3] It is considered to be on thesubgiant branch, contracting across theHertzsprung gap towards thered giant branch.[4]

In 1985, Jeffrey Hopkinset al. discovered that HR 9024 is a variable star, with a period of ~23.3 days.[7] It was given thevariable star designation OU Andromedae in 1986.[8] Paola Testaet al. reported that the star showedX-ray flare activity, in 2007.[9]

Fast rotation

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The spin rate of OU Andromedae is unusually high for anevolved star of this type, showing aprojected rotational velocity of 21.5 km/s. One possible explanation is that it may have engulfed a nearbygiant planet, such as ahot Jupiter, since aninfrared excess has been observed.[5] Another explanation relies on its strongmagnetic field; if OU Andromedae was anAp star during itsmain sequence stage of evolution, it could have retained both the strong magnetic field and the fast rotation of Ap stars.[4]

X-ray source

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OU Andromedae is a bright X-ray source, due to the activity of itscorona; it's estimated that solar-like active regions cover 30% of the surface. This is another effect of the strong magnetic field, which produces an uninterrupted flaring activity that generates a large volume of hot plasma at coronal temperatures (~7.5×106K).[10]

References

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  1. ^Argiroffi, C.; Reale, F.; Drake, J. J.; Ciaravella, A.; Testa, P.; Bonito, R.; Miceli, M.; Orlando, S.; Peres, G. (August 2019). "A stellar flare-coronal mass ejection event revealed by X-ray plasma motions".Nature Astronomy.3:742–748.arXiv:1905.11325.doi:10.1038/s41550-019-0781-4.S2CID 256704200.
  2. ^abcdefghVallenari, A.; et al. (Gaia collaboration) (2023)."Gaia Data Release 3. Summary of the content and survey properties".Astronomy and Astrophysics.674: A1.arXiv:2208.00211.Bibcode:2023A&A...674A...1G.doi:10.1051/0004-6361/202243940.S2CID 244398875. Gaia DR3 record for this source atVizieR.
  3. ^abcN. N. Samus; O. V. Durlevich; et al."OU And database entry".Combined General Catalog of Variable Stars (2017 ed.).CDS. Retrieved2018-11-12.
  4. ^abcdBorisova, A.; Aurière, M.; Petit, P.; Konstantinova-Antova, R.; Charbonnel, C.; Drake, N. A. (June 2016). "The different origins of magnetic fields and activity in the Hertzsprung gap stars, OU Andromedae and 31 Comae".Astronomy & Astrophysics.591: 15.arXiv:1604.07647.Bibcode:2016A&A...591A..57B.doi:10.1051/0004-6361/201526726.S2CID 55676875. A57.
  5. ^abcRodrigues da Silva, R.; et al. (March 2015). "On the Nature of Rapidly Rotating Single Evolved Stars".The Astrophysical Journal.801 (1): 6.arXiv:1503.03447.Bibcode:2015ApJ...801...54R.doi:10.1088/0004-637X/801/1/54.S2CID 119271718. 54.
  6. ^abcCutri, Roc M.; Skrutskie, Michael F.; Van Dyk, Schuyler D.; Beichman, Charles A.; Carpenter, John M.; Chester, Thomas; Cambresy, Laurent; Evans, Tracey E.; Fowler, John W.; Gizis, John E.; Howard, Elizabeth V.; Huchra, John P.; Jarrett, Thomas H.; Kopan, Eugene L.; Kirkpatrick, J. Davy; Light, Robert M.; Marsh, Kenneth A.; McCallon, Howard L.; Schneider, Stephen E.; Stiening, Rae; Sykes, Matthew J.; Weinberg, Martin D.; Wheaton, William A.; Wheelock, Sherry L.; Zacarias, N. (2003)."VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)".CDS/ADC Collection of Electronic Catalogues.2246: II/246.Bibcode:2003yCat.2246....0C.
  7. ^Hopkins, J. L.; Boyd, L. J.; Genet, R. M.; Hall, D. S. (March 1985)."Discovery of Variability in HR 9024"(PDF).Information Bulletin on Variable Stars.2684: 1.Bibcode:1985IBVS.2684....1H. Retrieved7 February 2023.
  8. ^Kholopov, P. N.; Samus, N. N.; Kazarovets, E. V.; Kireeva, N. N. (August 1987)."The 68th Name-List of Variable Stars"(PDF).Information Bulletin on Variable Stars.3058: 1.Bibcode:1987IBVS.3058....1K. Retrieved7 February 2023.
  9. ^Testa, Paola; Reale, Fabio; Garcia-Alvarez, David; Huenemoerder, David P. (July 2007)."Detailed Diagnostics of an X-Ray Flare in the Single Giant HR 9024".The Astrophysical Journal.663 (2):1232–1243.arXiv:astro-ph/0703422.Bibcode:2007ApJ...663.1232T.doi:10.1086/518241.S2CID 17916110. Retrieved7 February 2023.
  10. ^Gondoin, P. (October 2003), "The corona of HD 223460 (HR 9024)",Astronomy and Astrophysics,409:263–274,Bibcode:2003A&A...409..263G,doi:10.1051/0004-6361:20030978
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