Astronomy:Nu Phoenicis

From HandWiki
Short description: Star in the constellation Phoenix
Nu Phoenicis
Location of ν Phoenicis (circled)
Observation data
Equinox J2000.0]] (ICRS)
Constellation Phoenix
Right ascension  01h 15m 11.12143s[1]
Declination −45° 31′ 53.9926″[1]
Apparent magnitude (V) 4.95[2]
Characteristics
Spectral type F9 V Fe+0.4[3]
U−B color index +0.09[2]
B−V color index +0.57[2]
Astrometry
Radial velocity (Rv)+11.90±0.12[1] km/s
Proper motion (μ) RA: +665.086[1] mas/yr
Dec.: +178.070[1] mas/yr
Parallax (π)65.5270 ± 0.0704[1] mas
Distance49.77 ± 0.05 ly
(15.26 ± 0.02 pc)
Absolute magnitude (MV)4.07[4]
Details[5]
Mass1.15+0.03
−0.04 M☉
Radius1.26±0.02 R☉
Luminosity2.00+0.10
−0.09 L☉
Surface gravity (log g)4.340±0.030 cgs
Temperature6,116+46
−51 K
Metallicity [Fe/H]+0.16±0.06[4] dex
Rotational velocity (v sin i)3.7±0.5[4] km/s
Age3.9+1.7
−0.9 Gyr
Other designations
CD−46°346, GCTP 257.00, Gl 55, HD 7570, HIP 5862, HR 370, LHS 1220, LTT 696, SAO 215428[6]
Database references
SIMBADdata

Nu Phoenicis is a star in the southern constellation of Phoenix. It is visible to the naked eye with an apparent visual magnitude of 4.95.[2] This is a solar analogue, meaning its observed properties appear similar to the Sun, although it is somewhat more massive. At a distance of around 49.5 light years,[1] this star is located relatively near the Sun.

Based on observations of excess infrared radiation from this star, it may possess a dust ring that extends outward several AU from an inner edge starting at 10 AU.[7]

Properties

This is an F-type main-sequence star with a spectral type of F9V Fe+0.4,[3] indicating it is similar to the Sun but somewhat hotter and more luminous. The notation 'Fe+0.4' indicates strong iron absorption lines; the star is indeed metal-rich, with an iron abundance 45% greater than the Sun's. Nu Phoenicis has 1.15 times the solar mass and a radius of 1.26 times the solar radius. It is shining with 2.00 times the solar luminosity at an effective temperature of 6,116 K.[5]

Nu Phoenicis has a projected rotational velocity of 3.7 km/s,[4] and a low chromospheric activity index (log R′HK = −4.95).[8] These values indicate that the star is not particularly young and has an age of a few billion years; empirical calibrations estimate from the rotational velocity an age of 2.4 billion years, and from the activity index an age of 5.67 billion years.[8] Similarly, stellar evolution models estimate an age between 1 and 6 billion years, with a more probable value of 4.2 billion years.[9]

Nu Phoenicis has no known companions, and is considered to be a single star.[4] As a bright star similar to the Sun, it has been targeted in a number of studies searching for planets with the radial velocity method, but no detection has been made. High-precision observations with the HARPS spectrograph show that the radial velocity of the star has no significant variability, and is constant to 2.67 m/s, a value similar to the estimated jitter level of 2.48 m/s.[10] The star has also been included in the observations of the Anglo-Australian Planet Search, which did not find Jupiter-analogs with periods up to 6,000 days.[11]

Nu Phoenicis emits a significant amount of infrared excess, in comparison to the expected emission from the star's photosphere, indicating it has a circumstellar debris disk that is warmed by the star and emits thermal radiation.[7] The excess has been detected in long wavelengths, between 30[7] and 100 μm,[12] indicating relatively cold dust many astronomical units away from the star. Modeling the emission as a black body, the disk has an estimated temperature of 96 K and a radius of 12 AU, contributing to 0.00024% of the system's luminosity.[12]

See also

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 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. ↑ 2.0 2.1 2.2 2.3 Mermilliod, J.-C. (1986). "Compilation of Eggen's UBV data, transformed to UBV (unpublished)". Catalogue of Eggen's UBV Data. SIMBAD: 0. Bibcode: 1986EgUBV........0M. 
  3. ↑ 3.0 3.1 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 
  4. ↑ 4.0 4.1 4.2 4.3 4.4 Fuhrmann, K.; Chini, R.; Kaderhandt, L.; Chen, Z. (2017). "Multiplicity among Solar-type Stars". The Astrophysical Journal 836 (1): 139. doi:10.3847/1538-4357/836/1/139. Bibcode: 2017ApJ...836..139F. 
  5. ↑ 5.0 5.1 Harada, Caleb K. et al. (June 2024). "Setting the Stage for the Search for Life with the Habitable Worlds Observatory: Properties of 164 Promising Planet-survey Targets". The Astrophysical Journal Supplement Series 272 (2): id. 30. doi:10.3847/1538-4365/ad3e81. Bibcode: 2024ApJS..272...30H. 
  6. ↑ "nu. Phe -- High proper-motion Star". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-id?Ident=HD+7570. 
  7. ↑ 7.0 7.1 7.2 Beichman, C. A.; Tanner, A.; Bryden, G.; Stapelfeldt, K. R. et al. (2006). "IRS Spectra of Solar-Type Stars: A Search for Asteroid Belt Analogs". Astrophysical Journal 639 (2): 1166–1176. doi:10.1086/499424. Bibcode: 2006ApJ...639.1166B. 
  8. ↑ 8.0 8.1 Vican, Laura (June 2012). "Age Determination for 346 Nearby Stars in the Herschel DEBRIS Survey". The Astronomical Journal 143 (6): 135. doi:10.1088/0004-6256/143/6/135. Bibcode: 2012AJ....143..135V. 
  9. ↑ 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. 
  10. ↑ Zechmeister, M. et al. (2013). "The planet search programme at the ESO CES and HARPS. IV. The search for Jupiter analogues around solar-like stars". Astronomy & Astrophysics 592: A78. doi:10.1051/0004-6361/201116551. Bibcode: 2013A&A...552A..78Z. 
  11. ↑ Wittenmyer, Robert A.; Butler, R. P.; Tinney, C. G.; Horner, Jonathan; Carter, B. D.; Wright, D. J.; Jones, H. R. A.; Bailey, J. et al. (2016). "The Anglo-Australian Planet Search XXIV: The Frequency of Jupiter Analogs". The Astrophysical Journal 819 (1): 28. doi:10.3847/0004-637x/819/1/28. Bibcode: 2016ApJ...819...28W. 
  12. ↑ 12.0 12.1 Montesinos, B. et al. (September 2016). "Incidence of debris discs around FGK stars in the solar neighbourhood". Astronomy & Astrophysics 593: 31. doi:10.1051/0004-6361/201628329. A51. Bibcode: 2016A&A...593A..51M. 



Retrieved from "https://handwiki.org/wiki/index.php?title=Astronomy:Nu_Phoenicis&oldid=4131710"