Astronomy:Rho Phoenicis
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Phoenix |
| Right ascension | 00h 50m 41.186s[2] |
| Declination | −50° 59′ 12.54″[2] |
| Apparent magnitude (V) | 5.17 – 5.27[3] |
| Characteristics | |
| Spectral type | F3III[4] |
| U−B color index | 0.13[5] |
| B−V color index | 0.36[5] |
| Variable type | δ Scuti[3][5] |
| Astrometry | |
| Radial velocity (Rv) | 22.0[6] km/s |
| Proper motion (μ) | RA: 62.919[2] mas/yr Dec.: 44.139[2] mas/yr |
| Parallax (π) | 13.3180 ± 0.0629[2] mas |
| Distance | 245 ± 1 ly (75.1 ± 0.4 pc) |
| Absolute magnitude (MV) | +0.87[7] |
| Details | |
| Mass | 2.13[8] M☉ |
| Radius | 4.2[2] R☉ |
| Luminosity | 36[2] L☉ |
| Surface gravity (log g) | 3.52[8] cgs |
| Temperature | 6,917 ± 124[8] K |
| Metallicity [Fe/H] | −0.10[2] dex |
| Age | 1.00[8] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Rho Phoenicis (ρ Phoenicis) is a variable star in the constellation of Phoenix. From parallax measurements by the Gaia spacecraft, it is located at a distance of 245 light-years (75 parsecs) from Earth.
This star is classified as an F-type giant with a spectral type of F3III, and in the HR diagram it occupies in the lower part of the instability strip. Rho Phoenicis is Delta Scuti variable, changing its visual apparent magnitude between 5.17 and 5.27 with a period of around 0.1–0.2 days.[5][3] The pulsation period seems to vary in a timescale of weeks, which indicates the star is not a simple radial pulsator.[10] The analysis of the temperature variations over the pulsation cycles also supports this conclusion.[11] It is not clear if the pulsation period really is variable, or if the light curve is simply the sum of multiple stable pulsation frequencies.[12]
Stellar evolution models indicate that Rho Phoenicis has about 2.1 times the solar mass and an age of around 1 billion years.[8] This star is shining with 36 times the solar luminosity and has an effective temperature of 6,900 K.[8] Its metallicity is high, with an overall metal abundance 25% greater the solar value.[8] Gaia Data Release 2 discovered a star with the same proper motion and parallax as Rho Phoenicis. It has an apparent magnitude of 14.6 (G band) and is at a separation of 7.9 arcseconds.[13]
References
- ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. https://mast.stsci.edu/portal/Mashup/Clients/Mast/Portal.html.
- ↑ 2.0 2.1 2.2 2.3 2.4 2.5 2.6 2.7 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940 Gaia DR3 record for this source at VizieR.
- ↑ 3.0 3.1 3.2 Samus', N. N; Kazarovets, E. V; Durlevich, O. V; Kireeva, N. N; Pastukhova, E. N (2017). "General catalogue of variable stars: Version GCVS 5.1". Astronomy Reports 61 (1): 80. doi:10.1134/S1063772917010085. Bibcode: 2017ARep...61...80S.
- ↑ Houk, N. (1978). "Michigan atalogue of two dimensional spectral types for the HD stars, Vol. 2". Michigan Spectral Survey 2. Bibcode: 1978mcts.book.....H.
- ↑ 5.0 5.1 5.2 5.3 Garcia, J. R.; Cebral, J. R.; Scoccimarro, E. R.; Wahnon, P.; Arena, R.; Bazterra, V.; Pellizza, L.; Risi, A. et al. (1995). "A catalogue of variable stars in the lower instability strip". Astronomy and Astrophysics Supplement Series 109: 201. Bibcode: 1995A&AS..109..201G.
- ↑ Gontcharov, G. A. (November 2006). "Pulkovo Compilation of Radial Velocities for 35495 Hipparcos stars in a common system". Astronomy Letters 32 (11): 759–771. doi:10.1134/S1063773706110065. Bibcode: 2006AstL...32..759G.
- ↑ Holmberg, J.; Nordström, B.; Andersen, J. (2009). "The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics". Astronomy and Astrophysics 501 (3): 941. doi:10.1051/0004-6361/200811191. Bibcode: 2009A&A...501..941H.
- ↑ 8.0 8.1 8.2 8.3 8.4 8.5 8.6 Casagrande, L. et al. (June 2011). "New constraints on the chemical evolution of the solar neighbourhood and Galactic disc(s). Improved astrophysical parameters for the Geneva-Copenhagen Survey". Astronomy and Astrophysics 530: A138. doi:10.1051/0004-6361/201016276. Bibcode: 2011A&A...530A.138C.
- ↑ "Rho Phe". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=Rho+Phe.
- ↑ Smyth, M. J.; Stobie, R. S.; Shobbrook, R. R. (1975). "Frequency analysis of the three Delta Scuti stars BS 3265, 1653 and 242". Monthly Notices of the Royal Astronomical Society 171: 143–158. doi:10.1093/mnras/171.1.143. Bibcode: 1975MNRAS.171..143S.
- ↑ Sullivan, D. J.; Trodahl, H. J. (1978). "Temperature variations in rho Phe". Monthly Notices of the Royal Astronomical Society 183 (2): 201–204. doi:10.1093/mnras/183.2.201. Bibcode: 1978MNRAS.183..201S.
- ↑ Kurtz, D. W. (1980). "On the stability of observed frequencies in del SCT stars : A reanalysis of the Tuc". Monthly Notices of the Royal Astronomical Society 193: 61. doi:10.1093/mnras/193.1.61. Bibcode: 1980MNRAS.193...61K.
- ↑ Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G. Gaia DR2 record for this source at VizieR.
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