Rho Fornacis
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| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Fornax |
| Right ascension | 03h 47m 56.040s[1] |
| Declination | −30° 10′ 4.38″[1] |
| Apparent magnitude (V) | +5.54[2] |
| Characteristics | |
| Spectral type | G6III[1] |
| B−V color index | 0.98[2] |
| Astrometry | |
| Radial velocity (Rv) | 52.6 km/s |
| Proper motion (μ) | RA: +28[2] mas/yr Dec.: –230[2] mas/yr |
| Parallax (π) | 11.5326 ± 0.0512 mas[1] |
| Distance | 283 ± 1 ly (86.7 ± 0.4 pc) |
| Absolute magnitude (MV) | +0.85 |
| Other designations | |
| Database references | |
| SIMBAD | data |
Rho Fornacis (ρ For)[1] is a star of apparent magnitude +5.54 in the constellation of Fornax, the furnace. It is found, according to the new reduction of the parallax data from Hipparcos, to 269 light years of the Solar System.
Rho Fornacis is a yellow-orange giant of spectral type G6III[1][3] with an effective temperature of 4884 K.[4] It is similar, though somewhat hotter, than β Fornacis and π Fornacis, stars also in Fornax. The diameter of Rho Fornacis is 9.9 times larger than the solar diameter but its mass is barely 1% greater than that of the Sun. Its age is estimated at 5180 ± 3170 million years.
Rho Fornacis is a thick disk star, unlike most stars in our environment. Arcturus (α Boötis) and ε Fornacis, the latter in this same constellation, are examples of thick disk stars. The eccentricity of its orbit around the Galactic Center (e = 0.56) is considerably greater than that of the Sun (e = 0.16), star of the thin disk.[5] Consequently, it shows a low metallicity—relative abundance of elements heavier than helium—, less than half that of the solar ([Fe/H] = -0 ,35).[4] Elements such as aluminum, calcium and sodium are equally deficient. As in other similar stars, the oxygen/iron ratio is higher than in the Sun ([O/H] = 0.33).[6]
References
[edit]- ^ a b c d e f g =submit+id rho For -- Variable Star (SIMBAD)
- ^ a b c d "ρ Fornacis (rho Fornacis)". The Sky Live. Retrieved 28 September 2023.
- ^ "Rho Fornacis (Alcyone)". March 4, 2016. Archived from the original on 2016-03-04. Retrieved March 27, 2012.
- ^ a b da Silva, L.; Girardi, L. ; Pasquini, L. ; Setiawan, J.; von der Lühe, O.; de Medeiros, J. R. ; Hatzes, A. ; Döllinger, M.P.; Weiss, A. (1999). (2007). "Basic physical parameters of a selected sample of evolved stars". Astronomy & Astrophysics. 458. Bibcode:2006A&A...458..609D. pp. 609-623.
{{cite journal}}: CS1 maint: multiple names: authors list (link) CS1 maint: numeric names: authors list (link) - ^ Rho Fornacis (Ashland Astronomy Studio)[permanent dead link]
- ^ Alves-Brito, A.; Melendez, J.; Asplund , M. ; Ramirez, I.; Yong, D. (1999). Chemical similarities between the Galactic bulge and local thick disk red giants: O, Na, Mg, Al, Si, Ca, and Ti. Astronomy and Astrophysics. Vol. 513. Bibcode:2010A&A...513A..35A. A3.
{{cite book}}: CS1 maint: multiple names: authors list (link) CS1 maint: numeric names: authors list (link)
