Nu Phoenicis

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Nu Phoenicis
Phoenix constellation map.svg
Red circle.svg
Location of ν Phoenicis (circled)
Observation data
Epoch J2000       Equinox J2000
Constellation Phoenix
Right ascension 01h 15m 11.12150s [1]
Declination –45° 31′ 53.9954″ [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)+11.82 ± 0.15 [4]  km/s
Proper motion (μ)RA: 664.28 [4]   mas/yr
Dec.: 179.06 [4]   mas/yr
Parallax (π)65.8894 ± 0.1803  mas [4]
Distance 49.5 ± 0.1  ly
(15.18 ± 0.04  pc)
Absolute magnitude  (MV)4.07 [5]
Details [5]
Mass 1.17  M☉
Radius 1.26 ± 0.04  R☉
Luminosity 2.0 ± 0.1  L☉
Surface gravity (log g)4.31 ± 0.10  cgs
Temperature 6,066 ± 70  K
Metallicity [Fe/H]+0.16 ± 0.06  dex
Rotational velocity (v sin i)3.7 ± 0.5 km/s
Age 4.2 [6]   Gyr
Other designations
CD–46° 346, GCTP 257.00, Gl 55, HD 7570, HIP 5862, HR 370, LHS 1220, LTT 696, SAO  215428. [7]
Database references
SIMBAD data

Nu Phoenicis is a F-type main-sequence 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 an estimated distance of around 49.5  light years, [4] this star is located relatively near the Sun.

Contents

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. [8]

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 an estimated mass of 1.17 times the solar mass and a radius of 1.26 times the solar radius. It is shining with about double the solar luminosity at an effective temperature of 6,070  K. [5]

Nu Phoenicis has a projected rotational velocity of 3.7 km/s, [5] and a low chromospheric activity index (log R′HK = −4.95). [9] 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. [9] Similarly, stellar evolution models estimate an age between 1 and 6 billion years, with a more probable value of 4.2 billion years. [6]

Nu Phoenicis has no known companions, and is considered to be a single star. [5] 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. [8] The excess has been detected in long wavelengths, between 30 [8] 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

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<span class="mw-page-title-main">V538 Aurigae</span> Star in constellation Auriga

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<span class="mw-page-title-main">Nu Horologii</span> Star in the constellation Horologium

Nu Horologii, Latinized from ν Horologii, is the Bayer designation for a single star in the southern constellation of Horologium. It was catalogued by the Dutch explorer Frederick de Houtman in 1603. With an apparent visual magnitude of 5.3, this star can be seen with the naked eye from the southern hemisphere. Based upon parallax, Nu Horologii lies at a distance of 169 light-years from Earth. It is drifting closer to the Sun with a radial velocity of +31 km/s.

HD 219623 is a solitary star in the northern circumpolar constellation of Cassiopeia. HD 219623 is its Henry Draper Catalogue designation. It has an apparent visual magnitude of 5.59, which lies in the brightness range that is visible to the naked eye. According to the Bortle scale, it can be observed from dark suburban skies. Parallax measurements place it at an estimated distance of around 67.2 light years. It has a relatively high proper motion, advancing 262 mas per year across the celestial sphere.

c Ursae Majoris is the Bayer designation for a double-lined spectroscopic binary star system in the northern constellation of Ursa Major. It has an apparent visual magnitude of 5.18, which indicates that is visible to the naked eye. Parallax measurements yield an estimated distance of 66 light years from the Sun. The star is moving closer to the Earth with a heliocentric radial velocity of −14 km/s.

References

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  2. 1 2 3 4 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. 1 2 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, arXiv: astro-ph/0603770 , Bibcode:2006AJ....132..161G, doi:10.1086/504637, S2CID   119476992.
  4. 1 2 3 4 5 Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics . 616. A1. arXiv: 1804.09365 . Bibcode: 2018A&A...616A...1G . doi: 10.1051/0004-6361/201833051 .
  5. 1 2 3 4 5 Fuhrmann, K.; Chini, R.; Kaderhandt, L.; Chen, Z. (2017). "Multiplicity among Solar-type Stars". The Astrophysical Journal. 836 (1): 139. Bibcode:2017ApJ...836..139F. doi: 10.3847/1538-4357/836/1/139 .
  6. 1 2 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, arXiv: 1103.4651 , Bibcode:2011A&A...530A.138C, doi:10.1051/0004-6361/201016276, S2CID   56118016.
  7. ↑ "nu. Phe -- High proper-motion Star", SIMBAD Astronomical Database, Centre de Données astronomiques de Strasbourg , retrieved 2015-12-22.
  8. 1 2 3 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. arXiv: astro-ph/0601467 . Bibcode:2006ApJ...639.1166B. doi:10.1086/499424. S2CID   13493797.
  9. 1 2 Vican, Laura (June 2012), "Age Determination for 346 Nearby Stars in the Herschel DEBRIS Survey", The Astronomical Journal, 143 (6): 135, arXiv: 1203.1966 , Bibcode:2012AJ....143..135V, doi:10.1088/0004-6256/143/6/135, S2CID   118539505.
  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. arXiv: 1211.7263 . Bibcode:2013A&A...552A..78Z. doi:10.1051/0004-6361/201116551. S2CID   53694238.
  11. ↑ Wittenmyer, Robert A.; Butler, R. P.; Tinney, C. G.; Horner, Jonathan; Carter, B. D.; Wright, D. J.; Jones, H. R. A.; Bailey, J.; O'Toole, Simon J. (2016). "The Anglo-Australian Planet Search XXIV: The Frequency of Jupiter Analogs". The Astrophysical Journal. 819 (1): 28. arXiv: 1601.05465 . Bibcode:2016ApJ...819...28W. doi: 10.3847/0004-637x/819/1/28 . S2CID   118430306.
  12. 1 2 Montesinos, B.; et al. (September 2016), "Incidence of debris discs around FGK stars in the solar neighbourhood", Astronomy & Astrophysics, 593: 31, arXiv: 1605.05837 , Bibcode:2016A&A...593A..51M, doi:10.1051/0004-6361/201628329, S2CID   55251562, A51.
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