Astronomy:Delta Pavonis
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| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Pavo |
| Right ascension | 20h 08m 43.60887s[1] |
| Declination | −66° 10′ 55.4428″[1] |
| Apparent magnitude (V) | 3.56[2] |
| Characteristics | |
| Spectral type | G8 IV[3] |
| U−B color index | 0.45[2] |
| B−V color index | 0.76[2] |
| Variable type | Suspected[4] |
| Astrometry | |
| Radial velocity (Rv) | −23.52±0.81[5] km/s |
| Proper motion (μ) | RA: +1,211.761[1] mas/yr Dec.: –1,130.237[1] mas/yr |
| Parallax (π) | 163.9544 ± 0.1222[1] mas |
| Distance | 19.89 ± 0.01 ly (6.099 ± 0.005 pc) |
| Absolute magnitude (MV) | 4.62[6] |
| Details[7] | |
| Mass | 1.051±0.062[8] M☉ |
| Radius | 1.197±0.016 R☉ |
| Luminosity | 1.24±0.03 L☉ |
| Surface gravity (log g) | 4.26±0.06 cgs |
| Temperature | 5,571±48 K |
| Metallicity [Fe/H] | 0.33±0.03 dex |
| Rotation | 21.4±9.3 d[9] |
| Rotational velocity (v sin i) | 0.32 km/s |
| Age | 6.6–6.9[10] Gyr 9.3[6] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Delta Pavonis, Latinized from δ Pavonis, is a single[12] star in the southern constellation of Pavo. It has an apparent visual magnitude of 3.56,[11] making it a fourth-magnitude star that is visible to the naked eye from the southern hemisphere. Parallax measurements yield an estimated distance of 19.89 light-years (6.10 parsecs) from Earth.[1] This makes it one of the nearest bright stars to the Solar System. It is approaching the Sun with a radial velocity of −23.5 km/s, and is predicted to come as close as 17.8 light-years in around 49,200 years.[5]
Observations
This object is a subgiant of spectral type G8 IV; it will stop fusing hydrogen at its core relatively soon, starting the process of becoming a red giant. Hence, Delta Pavonis is 24% brighter than the Sun, but the effective temperature of its outer atmosphere is less: 5,571 K.[7] Its mass is 105% of Sol's mass, with a mean radius 120% of Sol's radius. Delta Pavonis's surface convection zone extends downward to about 43.1% of the star's radius, but only contains 4.8% of the star's mass.[13]
Spectroscopic examination of Delta Pavonis shows that it has a higher abundance of elements heavier than helium (metallicity) than does the Sun. This value is typically given in terms of the ratio of iron (chemical symbol Fe) to hydrogen (H) in a star's atmosphere, relative to that in Sol's atmosphere (iron being a good proxy for the presence of other heavy elements). The metallicity of Delta Pavonis is approximately
- [math]\displaystyle{ \begin{smallmatrix}\left [ \frac{Fe}{H} \right ]\ =\ 0.33\end{smallmatrix} }[/math]
This notation gives the logarithm of the iron-to-hydrogen ratio, relative to that of the Sun, meaning that Delta Pavonis's iron abundance is 214% of that of Sol. It is considered super metal-rich, and the high metallicity has slowed its evolution.[14] Studies have shown a correlation between abundant heavy elements in stars, and the presence of a planetary system,[15] so Delta Pavonis has a greater than average probability of harboring planets.[14]
The age of Delta Pavonis is approximately 6.6 to 6.9 billion years,[10] and is certainly in the 5 to 7 billion year range.[14] It appears to be rotating slowly, with a projected rotational velocity of 0.32 kilometers per second.[7]
Search for planets
The existence of a Jupiter-mass gas giant on a long-period orbit around Delta Pavonis is suspected, as of 2021, based on astrometric data.[16] A study in 2023 detected a trend in the star's radial velocity, which may indicate the presence of a planetary companion, supporting the previous astrometric result. Such a planet would, at minimum, orbit with a period of 37 years at a distance of 11.1 astronomical unit|AU, and have a mass at least 69 M⊕ (0.22 |♃|J}}}}}}).[9]
SETI
Delta Pavonis has been identified by Maggie Turnbull and Jill Tarter of the SETI Institute as the "Best SETI target" among the 100 closest G-type stars. Properties in its favor include a high metallicity, minimal level of magnetic activity, low rotation rate, and kinematic membership in the thin disk population of the Milky Way. Gas giants orbiting in, near, or through a star's habitable zone may destabilize the orbits of terrestrial planets in that zone; the lack of detected radial velocity variation suggests that there are no such gas giants orbiting Delta Pavonis. However, observation has detected no artificial radio sources.[17] Delta Pavonis, a close photometric match to the Sun, is the nearest solar analog that is not a member of a binary or multiple star system.[14]
References
- ↑ 1.0 1.1 1.2 1.3 1.4 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.
- ↑ 2.0 2.1 2.2 Cousins, A. W. J.; Stoy, R. H. (1962). "Photoelectric magnitudes and colours of Southern stars". Royal Observatory Bulletin 64: 103–248. Bibcode: 1962RGOB...64..103C.
- ↑ Gray, R. O. et al. (July 2006), "Contributions to the Nearby Stars (NStars) Project: spectroscopy of stars earlier than M0 within 40 pc-The Southern Sample", The Astronomical Journal 132 (1): 161–170, doi:10.1086/504637, Bibcode: 2006AJ....132..161G.
- ↑ Ruban, E. V. et al. (September 2006), "Spectrophotometric observations of variable stars", Astronomy Letters 32 (9): 604–607, doi:10.1134/S1063773706090052, Bibcode: 2006AstL...32..604R
- ↑ 5.0 5.1 Bailer-Jones, C.A.L. et al. (2018). "New stellar encounters discovered in the second Gaia data release". Astronomy & Astrophysics 616: A37. doi:10.1051/0004-6361/201833456. Bibcode: 2018A&A...616A..37B.
- ↑ 6.0 6.1 Holmberg, J.; Nordström, B.; Andersen, J. (July 2009), "The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics", Astronomy and Astrophysics 501 (3): 941–947, doi:10.1051/0004-6361/200811191, Bibcode: 2009A&A...501..941H.
- ↑ 7.0 7.1 7.2 Rains, Adam D. et al. (April 2020). "Precision angular diameters for 16 southern stars with VLTI/PIONIER". Monthly Notices of the Royal Astronomical Society 493 (2): 2377–2394. doi:10.1093/mnras/staa282. Bibcode: 2020MNRAS.493.2377R.
- ↑ Pinheiro, F. J. G. et al. (December 2014), "On the mass estimation for FGK stars: comparison of several methods", Monthly Notices of the Royal Astronomical Society 445 (3): 2223–2231, doi:10.1093/mnras/stu1812, Bibcode: 2014MNRAS.445.2223P.
- ↑ 9.0 9.1 Laliotis, Katherine et al. (February 2023). "Doppler Constraints on Planetary Companions to Nearby Sun-like Stars: An Archival Radial Velocity Survey of Southern Targets for Proposed NASA Direct Imaging Missions". The Astronomical Journal 165 (4): 176. doi:10.3847/1538-3881/acc067. Bibcode: 2023AJ....165..176L.
- ↑ 10.0 10.1 Mamajek, Eric E.; Hillenbrand, Lynne A. (November 2008). "Improved Age Estimation for Solar-Type Dwarfs Using Activity-Rotation Diagnostics". The Astrophysical Journal 687 (2): 1264–1293. doi:10.1086/591785. Bibcode: 2008ApJ...687.1264M.
- ↑ 11.0 11.1 "NSV 12790 -- Variable Star". SIMBAD. Centre de Données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-id?Ident=HD+190248.
- ↑ Fuhrmann, K. et al. (February 2017). "Multiplicity among Solar-type Stars". The Astrophysical Journal 836 (1): 23. doi:10.3847/1538-4357/836/1/139. 139. Bibcode: 2017ApJ...836..139F.
- ↑ Takeda, G.; Ford, E. B.; Sills, A.; Rasio, F. A.; Fischer, D. A.; Valenti, J. A. (November 2008). "Stellar parameters of nearby cool stars (Takeda+, 2007)". VizieR On-line Data Catalog 216: 80297. doi:10.26093/cds/vizier.21680297. J/ApJS/168/297. Originally Published in: 2007ApJS..168..297T. Bibcode: 2008yCat..21680297T.
- ↑ 14.0 14.1 14.2 14.3 G. F. Porto de Mello; E. F. del Peloso; L. Ghezzi (2006). "Astrobiologically interesting stars within 10 parsecs of the Sun". Astrobiology 6 (2): 308–331. doi:10.1089/ast.2006.6.308. PMID 16689649. Bibcode: 2006AsBio...6..308P.
- ↑ Sousa, S.G. et al. (2006). "Spectroscopic parameters for a sample of metal-rich solar-type stars". Astronomy and Astrophysics 458 (3): 873–880. doi:10.1051/0004-6361:20065658. Bibcode: 2006A&A...458..873S.
- ↑ Makarov, Valeri V. et al. (2021). "Looking for Astrometric Signals below 20 m/s: A Candidate Exo-Jupiter in δ Pav". Research Notes of the AAS 5 (5): 108. doi:10.3847/2515-5172/abfec9. ISSN 2515-5172. Bibcode: 2021RNAAS...5..108M.
- ↑ M.C. Turnbull; J.C. Tarter (2003). "Target Selection for SETI. II. Tycho-2 Dwarfs, Old Open Clusters, and the Nearest 100 Stars". The Astrophysical Journal Supplement Series 149 (2): 423–436. doi:10.1086/379320. Bibcode: 2003ApJS..149..423T.
Further reading
- Bell, R. A. (1973), "The carbon abundance and colours of Delta Pavonis", Monthly Notices of the Royal Astronomical Society 162: 37, doi:10.1093/mnras/162.1.37, Bibcode: 1973MNRAS.162...37B.
- Harmer, D. L. et al. (1970), "The composition of delta Pavonis", Monthly Notices of the Royal Astronomical Society 150: 409, doi:10.1093/mnras/150.4.409, Bibcode: 1970MNRAS.150..409H.
- Rodgers, A. W. (1969), "The composition and age of δ Pavonis", Monthly Notices of the Royal Astronomical Society 145 (2): 151, doi:10.1093/mnras/145.2.151, Bibcode: 1969MNRAS.145..151R.
External links
- "Delta Pavonis". SolStation. http://www.solstation.com/stars/dpavonis.htm.
Coordinates: 
20h 08m 43.6084s, −66° 10′ 55.446″
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