Rho Tauri
| Rho Tauri (ρ) | |
 | |
| Observationsdata Epok: J2000.0 | |
|---|---|
| Stjärnbild | Oxen |
| Rektascension | 04t 33m 50,91753s[1] |
| Deklination | 14° 50′ 39,9232″[1] |
| Skenbar magnitud () | +4,66[2] |
| Stjärntyp | |
| Spektraltyp | A8V[3] |
| U–B | +0,09[2] |
| B–V | +0,24[2] |
| Variabeltyp | Pulserande variabel av Delta Scuti-typ[4] |
| Astrometri | |
| Radialhastighet () | +39,6[5] km/s |
| Egenrörelse (µ) | RA: 103,20[1] mas/år Dek.: -26,48[1] mas/år |
| Parallax () | 20,61 ± 0,57[1] |
| Avstånd | 158 ± 4 lå (59 ± 1 pc) |
| Absolut magnitud () | +1,26[6] |
| Detaljer | |
| Massa | 1,88[6] eller 2,09 ± 0,21[7] M☉ |
| Luminositet | 1,39[7] L☉ |
| Temperatur | 7 640[7] K |
| Vinkelhastighet | 117[6] km/s |
| Andra beteckningar | |
| ρ Tauri, 86 Tauri, BD + 14 720, FK5 1125, HD 28910, HIP 21273, HR 1444, SAO 94007 [8] | |
Rho Tauri (ρ Tauri , förkortat Rho Tau, ρ Tau) som är stjärnans Bayerbeteckning, är en stjärna belägen i den mellersta delen av stjärnbilden Oxen och ingår i stjärnhopen Hyaderna.[7] Den har en skenbar magnitud på 4,66[2] och är synlig för blotta ögat. Baserat på parallaxmätning inom Hipparcosuppdraget på ca 20,6 mas,[1] beräknas den befinna sig på ett avstånd av ca 158 ljusår (49 parsek) från solen.
Hyaderna, med ρ Tauri som en blå stjärna till vänster om centrum.
Egenskaper
Rho Tauri är en blå stjärna i huvudserien av spektralklass A8V[3]. Den har en massa som är dubbelt så stor som solens massa[7] och utsänder från dess fotosfär ca 1,4[7] gånger mera energi än solen vid en effektiv temperatur på ca 7 640[7] K. Den klassificeras som en Delta Scuti-variabel[7] och varierar i magnitud med 0,010 enheter över en period av 1,61 timmar.[4]
Källor
- Den här artikeln är helt eller delvis baserad på material från engelskspråkiga Wikipedia, tidigare version.
Referenser
- ^ [a b c d e f] van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, Bibcode:2007A&A...474..653V, arXiv:0708.1752 , doi:10.1051/0004-6361:20078357
- ^ [a b c d] Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV data, SIMBAD, Bibcode:1986EgUBV........0M.
- ^ [a b] Cowley, A.; et al. (April 1969), "A study of the bright A stars. I. A catalogue of spectral classifications", Astronomical Journal, 74: 375–406, Bibcode:1969AJ.....74..375C, doi:10.1086/110819.
- ^ [a b] Solano, E.; Fernley, J. (April 1997), "Spectroscopic survey of delta Scuti stars. I. Rotation velocities and effective temperatures", A & A Supplement series, 122: 131−147, Bibcode:1997A&AS..122..131S, doi:10.1051/aas:1997329.
- ^ Evans, D. S. (June 20–24, 1966), "The Revision of the General Catalogue of Radial Velocities", in Batten, Alan Henry; Heard, John Frederick, Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30, University of Toronto: International Astronomical Union, Bibcode:1967IAUS...30...57E.
- ^ [a b c] Pizzolato, N.; et al. (September 2000), "Evolution of X-ray activity of 1-3 Msun late-type stars in early post-main-sequence phases", Astronomy and Astrophysics, 361: 614–628, Bibcode:2000A&A...361..614P.
- ^ [a b c d e f g h] Gebran, M.; et al. (November 2010), "Chemical composition of A and F dwarfs members of the Hyades open cluster", Astronomy and Astrophysics, 523: A71, Bibcode:2010A&A...523A..71G, arXiv:1006.5284 , doi:10.1051/0004-6361/200913273.
- ^ "rho Tau -- Variable Star of delta Sct type", SIMBAD, Centre de Données astronomiques de Strasbourg, hämtad 2014-12-28
Externa länkar
Media som används på denna webbplats
Taurus IAU.svg
Författare/Upphovsman: IAU and Sky & Telescope magazine (Roger Sinnott & Rick Fienberg), Licens: CC BY 3.0
IAU Taurus chart
Författare/Upphovsman: IAU and Sky & Telescope magazine (Roger Sinnott & Rick Fienberg), Licens: CC BY 3.0
IAU Taurus chart
Hyades cluster.jpg
Författare/Upphovsman: NASA, ESA, and STScI, Licens: CC BY-SA 4.0
This image shows the Hyades star cluster, the nearest cluster to us. The Hyades cluster is very well studied due to its location, but previous searches for planets have produced only one. A new study led by Jay Farihi of the University of Cambridge, UK, has now found the atmospheres of two burnt-out stars in this cluster — known as white dwarfs — to be “polluted” by rocky debris circling the star. Seeing evidence of asteroids points to the possibility of Earth-sized planets in the same system, as asteroids are the building blocks of major planets. Planet-forming processes are inefficient, and spawn many times more small bodies than large bodies — but once rocky embryos the size of asteroids are built, planets are sure to follow.
Författare/Upphovsman: NASA, ESA, and STScI, Licens: CC BY-SA 4.0
This image shows the Hyades star cluster, the nearest cluster to us. The Hyades cluster is very well studied due to its location, but previous searches for planets have produced only one. A new study led by Jay Farihi of the University of Cambridge, UK, has now found the atmospheres of two burnt-out stars in this cluster — known as white dwarfs — to be “polluted” by rocky debris circling the star. Seeing evidence of asteroids points to the possibility of Earth-sized planets in the same system, as asteroids are the building blocks of major planets. Planet-forming processes are inefficient, and spawn many times more small bodies than large bodies — but once rocky embryos the size of asteroids are built, planets are sure to follow.