HD 74772

	HD 74772
Observationsdata; Epok: J2000.0
Stjärnbild	Seglet
Rektascension	08t 44m 23,94539s
Deklination	-42° 38′ 57,3933″
Skenbar magnitud ()	+4,05 (V)
Stjärntyp
Spektraltyp	G6 III
B–V	+0,874 ± 0,002
Astrometri
Radialhastighet ()	-2,0 ± 0,3 km/s
Egenrörelse (µ)	RA: -22,641 mas/år; Dek.: +19,137 mas/år
Parallax ()	15,7791 ± 0,3148
Avstånd	207 ± 4 lå (63 ± 1 pc)
Absolut magnitud ()	-0,18
Detaljer
Massa	3,2 M☉
Radie	12 R☉
Luminositet	128,02 L☉
Temperatur	5 210 K
Metallicitet	-0,03 (Fe/H) dex
Vinkelhastighet	5,8 km/s
Andra beteckningar
	AKARI-IRC-V1, J0844239-423857, CCDM J08444-4239A, CD-42 4569, CPD-42 2878, GJ 9276, GJ 321.1, GSC 07683-02233, HD 74772, HIC 42884, HIP 42884, HR 3477, IRAS 08426-4228, 2MASS J08442396-4238572, PLX 2092, PPM 313500, SAO 220371, TD1 13030, TYC 7683-2233-1, WDS J08444-4239A, Gaia DR2 5524834518402672896

HD 74772 är en ensam stjärna^[11] belägen i den norra delen av stjärnbilden Seglet och som också har Bayer-beteckningen d Velorum. Den befinner sig nära Vela SNR, vilket ger en intensiv bakgrund av röntgenstrålning.^[12] Den har en skenbar magnitud av ca 4,05^[2] och är svagt synlig för blotta ögat där ljusföroreningar ej förekommer. Baserat på parallax enligt Gaia Data Release 2 på ca 15,8^[1] mas, beräknas den befinna sig på ett avstånd på ca 207 ljusår (ca 63 parsek) från solen. Den rör sig närmare solen med en heliocentrisk radialhastighet på ca -2 km/s.^[4]

Egenskaper

HD 74772 är en gul till vit jättestjärna av spektralklass G6 III.^[3] Den har en massa som är ca 3^[5] solmassor, en radie, som baserat på en uppmätt vinkeldiameter av 1,73 ± 0,12 mas,^[13] är ca 12^[6] solradier och har ca 128 gånger solens utstrålning av energi^[2] från dess fotosfär vid en effektiv temperatur av ca 5 200 K.^[7]

Referenser

Den här artikeln är helt eller delvis baserad på material från engelskspråkiga Wikipedia, HD 74772, 19 december 2020.

Noter

^ [a b c d e f] Brown, 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 at VizieR.
^ [a b c d e f] Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv:1108.4971, Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015.
^ [a b] Keenan, Philip C.; McNeil, Raymond C. (1989), "The Perkins catalog of revised MK types for the cooler stars", Astrophysical Journal Supplement Series, 71: 245, Bibcode:1989ApJS...71..245K, doi:10.1086/191373.
^ [a b] de Bruijne, J. H. J.; Eilers, A.-C. (October 2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project", Astronomy & Astrophysics, 546: 14, arXiv:1208.3048, Bibcode:2012A&A...546A..61D, doi:10.1051/0004-6361/201219219, A61.
^ [a b] Gondoin, P. (December 1999), "Evolution of X-ray activity and rotation on G-K giants", Astronomy and Astrophysics, 352: 217–227, Bibcode:1999A&A...352..217G.
^ [a b] Lang, Kenneth R. (2006), Astrophysical formulae, Astronomy and astrophysics library, 1 (3rd ed.), Birkhäuser, ISBN 3-540-29692-1. The radius (R*) is given by:
${\begin{aligned}2\cdot R_{*}&={\frac {(10^{-3}\cdot 63.4\cdot 1.73)\ {\text{AU}}}{0.0046491\ {\text{AU}}/R_{\bigodot }}}\\&\approx 23.6\cdot R_{\bigodot }\end{aligned}}$
^ [a b c] Jones, K. L.; et al. (June 1992), "Spectroscopic investigation of cool giants and the authenticity of their reported microwave emission", Monthly Notices of the Royal Astronomical Society, 256 (3): 535–544, Bibcode:1992MNRAS.256..535J, doi:10.1093/mnras/256.3.535.
^ de Medeiros, J. R.; Mayor, M. (October 1995), "On the link between rotation and coronal activity in evolved stars", Astronomy and Astrophysics, 302: 745, Bibcode:1995A&A...302..745D.
^ http://simbad.u-strasbg.fr/simbad/sim-id?Ident=HD+74772 |Hämtad 2020-12-18.
^ "HD 74772". SIMBAD. Centre de données astronomiques de Strasbourg. Hämtad 2018-08-07.
^ Eggleton, P. P.; Tokovinin, A. A. (2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x.
^ Maggio, A.; et al. (1993), "Soft X-ray Emission and Spectra of Evolved Stars from ROSAT Pointed Observations", in Linsky, Jeffrey L.; Serio, Salvatore (eds.), Physics of Solar and Stellar Coronae: G. S. Vaiana Memorial Symposium, held 22-26 June, 1992, in Palermo, Italy, Astrophysics and Space Science Library, 183, P. O. Box 17, 3300 AA Dordrecht, The Netherlands: Kluwer Academoc Publishers, p. 365, Bibcode:1993ASSL..183..365M, doi:10.1007/978-94-011-1964-1_47.
^ Richichi, A.; et al. (February 2005), "CHARM2: An updated Catalog of High Angular Resolution Measurements", Astronomy and Astrophysics, 431 (2): 773–777, Bibcode:2005A&A...431..773R, doi:10.1051/0004-6361:20042039.

Externa länkar

https://www.universeguide.com/star/42884/hd74772.

[A-1] [a b c d e f] Brown, 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 at VizieR.

[B-2] [a b c d e f] Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv:1108.4971, Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015.

[C-3] [a b] Keenan, Philip C.; McNeil, Raymond C. (1989), "The Perkins catalog of revised MK types for the cooler stars", Astrophysical Journal Supplement Series, 71: 245, Bibcode:1989ApJS...71..245K, doi:10.1086/191373.

[D-4] [a b] de Bruijne, J. H. J.; Eilers, A.-C. (October 2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project", Astronomy & Astrophysics, 546: 14, arXiv:1208.3048, Bibcode:2012A&A...546A..61D, doi:10.1051/0004-6361/201219219, A61.

[E-5] [a b] Gondoin, P. (December 1999), "Evolution of X-ray activity and rotation on G-K giants", Astronomy and Astrophysics, 352: 217–227, Bibcode:1999A&A...352..217G.

[F-6] [a b] Lang, Kenneth R. (2006), Astrophysical formulae, Astronomy and astrophysics library, 1 (3rd ed.), Birkhäuser, ISBN 3-540-29692-1. The radius (R*) is given by:
${\begin{aligned}2\cdot R_{*}&={\frac {(10^{-3}\cdot 63.4\cdot 1.73)\ {\text{AU}}}{0.0046491\ {\text{AU}}/R_{\bigodot }}}\\&\approx 23.6\cdot R_{\bigodot }\end{aligned}}$

[G-7] [a b c] Jones, K. L.; et al. (June 1992), "Spectroscopic investigation of cool giants and the authenticity of their reported microwave emission", Monthly Notices of the Royal Astronomical Society, 256 (3): 535–544, Bibcode:1992MNRAS.256..535J, doi:10.1093/mnras/256.3.535.

[H-8] Medeiros, J. R.; Mayor, M. (October 1995), "On the link between rotation and coronal activity in evolved stars", Astronomy and Astrophysics, 302: 745, Bibcode:1995A&A...302..745D.

[SIMBAD-9] ttp://simbad.u-strasbg.fr/simbad/sim-id?Ident=HD+74772 |Hämtad 2020-12-18.

[I-10] "HD 74772". SIMBAD. Centre de données astronomiques de Strasbourg. Hämtad 2018-08-07.

[J-11] Eggleton, P. P.; Tokovinin, A. A. (2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x.

[K-12] Maggio, A.; et al. (1993), "Soft X-ray Emission and Spectra of Evolved Stars from ROSAT Pointed Observations", in Linsky, Jeffrey L.; Serio, Salvatore (eds.), Physics of Solar and Stellar Coronae: G. S. Vaiana Memorial Symposium, held 22-26 June, 1992, in Palermo, Italy, Astrophysics and Space Science Library, 183, P. O. Box 17, 3300 AA Dordrecht, The Netherlands: Kluwer Academoc Publishers, p. 365, Bibcode:1993ASSL..183..365M, doi:10.1007/978-94-011-1964-1_47.

[L-13] Richichi, A.; et al. (February 2005), "CHARM2: An updated Catalog of High Angular Resolution Measurements", Astronomy and Astrophysics, 431 (2): 773–777, Bibcode:2005A&A...431..773R, doi:10.1051/0004-6361:20042039.

[1]

[2]

[3]

[4]

[5]

[6]

[7]

[8]

[9]

[10]

[11]

[12]

[13]