  | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Auriga |
| Right ascension | 06h 46m 44.3388s [1] |
| Declination | +43° 34′ 38.737″ [1] |
| Apparent magnitude (V) | 5.25 [2] |
| Characteristics | |
| Spectral type | G0 V [3] |
| U−B color index | +0.06 [2] |
| B−V color index | +0.570 [4] |
| Astrometry | |
| Radial velocity (Rv) | –24 [5] km/s |
| Proper motion (μ) |
RA: –1.07
[1]
mas/
yr Dec.: +164.25 [1] mas/ yr |
| Parallax (π) | 60.56 ± 0.73 mas [1] |
| Distance | 53.9 ± 0.6
ly (16.5 ± 0.2 pc) |
| Absolute magnitude (MV) | 4.13 [5] |
| Details | |
| Mass | 1.079 [6] M☉ |
| Radius | 1.18 [6] R☉ |
| Surface gravity (log g) | 4.06 [3] cgs |
| Temperature | 5,989 [3] K |
| Metallicity [Fe/H] | +0.05 [3] dex |
| Rotational velocity (v sin i) | 5.03 [4] km/s |
| Age | 3.2 [5] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Psi5 Aurigae (ψ5 Aur, ψ5 Aurigae) is a star [8] in the northern constellation of Auriga. It is faintly visible to the naked eye with an apparent visual magnitude of 5.25. [2] Based upon parallax measurements made during the Hipparcos mission, this star is approximately 53.9 light-years (16.5 parsecs) distant from Earth. [1] There is an optical companion [8] which is 36 arcseconds away and has an apparent magnitude of +8.4.
It used to be known to be part of a much bigger constellation named Telescopium Herschelii before it was unrecognized by the International Astronomical Union (IAU).
Characteristics
The spectrum of this star shows it to be a G-type main sequence star with a stellar classification of G0 V. [3] Thought to be around 4 billion years old, it is similar in size, mass, [6] and composition to the Sun, [3] making this a solar analog. It is radiating energy into space at an effective temperature of 5,989 K, [3] giving it the golden-hued glow of a G-type star. [9]
Debris disk
Observation in the infrared shows an excess emission that suggests the presence of a circumstellar disk of dust, known as a debris disk. This material has a mean temperature of 60 K, indicating that it is orbiting at a distance of about 29 astronomical units from the host star. The dust has about half the mass of the Moon and is around 600 million years old. [10] The star is being examined for evidence of extrasolar planets, [11] but none have been found so far.
See also
References
- ^ a b c d e f van Leeuwen, Floor (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv: 0708.1752v1, Bibcode: 2007A&A...474..653V, doi: 10.1051/0004-6361:20078357, S2CID 18759600. Note: see VizieR catalogue I/311.
- ^ a b c Argue, A. N. (1966), "UBV photometry of 550 F, G and K type stars", Monthly Notices of the Royal Astronomical Society, 133 (4): 475, Bibcode: 1966MNRAS.133..475A, doi: 10.1093/mnras/133.4.475.
- ^ a b c d e f g Cenarro, A. J.; et al. (January 2007), "Medium-resolution Isaac Newton Telescope library of empirical spectra - II. The stellar atmospheric parameters", Monthly Notices of the Royal Astronomical Society, 374 (2): 664–690, arXiv: astro-ph/0611618, Bibcode: 2007MNRAS.374..664C, doi: 10.1111/j.1365-2966.2006.11196.x, S2CID 119428437.
- ^ a b Martínez–Arnáiz, R.; et al. (September 2010), "Chromospheric activity and rotation of FGK stars in the solar vicinity. An estimation of the radial velocity jitter" (PDF), Astronomy and Astrophysics, 520: A79, arXiv: 1002.4391, Bibcode: 2010A&A...520A..79M, doi: 10.1051/0004-6361/200913725, S2CID 43455849, archived from the original (PDF) on 2017-09-22, retrieved 2018-11-04.
- ^ a b c 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, arXiv: 0811.3982, Bibcode: 2009A&A...501..941H, doi: 10.1051/0004-6361/200811191, S2CID 118577511.
- ^ a b c Takeda, Genya; et al. (February 2007), "Structure and Evolution of Nearby Stars with Planets. II. Physical Properties of ~1000 Cool Stars from the SPOCS Catalog", The Astrophysical Journal Supplement Series, 168 (2): 297–318, arXiv: astro-ph/0607235, Bibcode: 2007ApJS..168..297T, doi: 10.1086/509763, S2CID 18775378.
- ^ "psi05 Aur". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2012-08-24.
- ^ a b Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869–879, arXiv: 0806.2878, Bibcode: 2008MNRAS.389..869E, doi: 10.1111/j.1365-2966.2008.13596.x, S2CID 14878976.
- ^ "The Colour of Stars", Australia Telescope, Outreach and Education, Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, archived from the original on March 18, 2012, retrieved 2012-01-16.
- ^ Rodriguez, David R.; Zuckerman, B. (February 2012), "Binaries among Debris Disk Stars", The Astrophysical Journal, 745 (2): 147, arXiv: 1111.5618, Bibcode: 2012ApJ...745..147R, doi: 10.1088/0004-637X/745/2/147, S2CID 73681879.
- ^ Grether, Daniel; Lineweaver, Charles H. (April 2006), "How Dry is the Brown Dwarf Desert? Quantifying the Relative Number of Planets, Brown Dwarfs, and Stellar Companions around Nearby Sun-like Stars", The Astrophysical Journal, 640 (2): 1051–1062, arXiv: astro-ph/0412356, Bibcode: 2006ApJ...640.1051G, doi: 10.1086/500161, S2CID 8563521.
External links
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| |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Auriga |
| Right ascension | 06h 46m 44.3388s [1] |
| Declination | +43° 34′ 38.737″ [1] |
| Apparent magnitude (V) | 5.25 [2] |
| Characteristics | |
| Spectral type | G0 V [3] |
| U−B color index | +0.06 [2] |
| B−V color index | +0.570 [4] |
| Astrometry | |
| Radial velocity (Rv) | –24 [5] km/s |
| Proper motion (μ) |
RA: –1.07
[1]
mas/
yr Dec.: +164.25 [1] mas/ yr |
| Parallax (π) | 60.56 ± 0.73 mas [1] |
| Distance | 53.9 ± 0.6
ly (16.5 ± 0.2 pc) |
| Absolute magnitude (MV) | 4.13 [5] |
| Details | |
| Mass | 1.079 [6] M☉ |
| Radius | 1.18 [6] R☉ |
| Surface gravity (log g) | 4.06 [3] cgs |
| Temperature | 5,989 [3] K |
| Metallicity [Fe/H] | +0.05 [3] dex |
| Rotational velocity (v sin i) | 5.03 [4] km/s |
| Age | 3.2 [5] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Psi5 Aurigae (ψ5 Aur, ψ5 Aurigae) is a star [8] in the northern constellation of Auriga. It is faintly visible to the naked eye with an apparent visual magnitude of 5.25. [2] Based upon parallax measurements made during the Hipparcos mission, this star is approximately 53.9 light-years (16.5 parsecs) distant from Earth. [1] There is an optical companion [8] which is 36 arcseconds away and has an apparent magnitude of +8.4.
It used to be known to be part of a much bigger constellation named Telescopium Herschelii before it was unrecognized by the International Astronomical Union (IAU).
Characteristics
The spectrum of this star shows it to be a G-type main sequence star with a stellar classification of G0 V. [3] Thought to be around 4 billion years old, it is similar in size, mass, [6] and composition to the Sun, [3] making this a solar analog. It is radiating energy into space at an effective temperature of 5,989 K, [3] giving it the golden-hued glow of a G-type star. [9]
Debris disk
Observation in the infrared shows an excess emission that suggests the presence of a circumstellar disk of dust, known as a debris disk. This material has a mean temperature of 60 K, indicating that it is orbiting at a distance of about 29 astronomical units from the host star. The dust has about half the mass of the Moon and is around 600 million years old. [10] The star is being examined for evidence of extrasolar planets, [11] but none have been found so far.
See also
References
- ^ a b c d e f van Leeuwen, Floor (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv: 0708.1752v1, Bibcode: 2007A&A...474..653V, doi: 10.1051/0004-6361:20078357, S2CID 18759600. Note: see VizieR catalogue I/311.
- ^ a b c Argue, A. N. (1966), "UBV photometry of 550 F, G and K type stars", Monthly Notices of the Royal Astronomical Society, 133 (4): 475, Bibcode: 1966MNRAS.133..475A, doi: 10.1093/mnras/133.4.475.
- ^ a b c d e f g Cenarro, A. J.; et al. (January 2007), "Medium-resolution Isaac Newton Telescope library of empirical spectra - II. The stellar atmospheric parameters", Monthly Notices of the Royal Astronomical Society, 374 (2): 664–690, arXiv: astro-ph/0611618, Bibcode: 2007MNRAS.374..664C, doi: 10.1111/j.1365-2966.2006.11196.x, S2CID 119428437.
- ^ a b Martínez–Arnáiz, R.; et al. (September 2010), "Chromospheric activity and rotation of FGK stars in the solar vicinity. An estimation of the radial velocity jitter" (PDF), Astronomy and Astrophysics, 520: A79, arXiv: 1002.4391, Bibcode: 2010A&A...520A..79M, doi: 10.1051/0004-6361/200913725, S2CID 43455849, archived from the original (PDF) on 2017-09-22, retrieved 2018-11-04.
- ^ a b c 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, arXiv: 0811.3982, Bibcode: 2009A&A...501..941H, doi: 10.1051/0004-6361/200811191, S2CID 118577511.
- ^ a b c Takeda, Genya; et al. (February 2007), "Structure and Evolution of Nearby Stars with Planets. II. Physical Properties of ~1000 Cool Stars from the SPOCS Catalog", The Astrophysical Journal Supplement Series, 168 (2): 297–318, arXiv: astro-ph/0607235, Bibcode: 2007ApJS..168..297T, doi: 10.1086/509763, S2CID 18775378.
- ^ "psi05 Aur". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2012-08-24.
- ^ a b Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869–879, arXiv: 0806.2878, Bibcode: 2008MNRAS.389..869E, doi: 10.1111/j.1365-2966.2008.13596.x, S2CID 14878976.
- ^ "The Colour of Stars", Australia Telescope, Outreach and Education, Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, archived from the original on March 18, 2012, retrieved 2012-01-16.
- ^ Rodriguez, David R.; Zuckerman, B. (February 2012), "Binaries among Debris Disk Stars", The Astrophysical Journal, 745 (2): 147, arXiv: 1111.5618, Bibcode: 2012ApJ...745..147R, doi: 10.1088/0004-637X/745/2/147, S2CID 73681879.
- ^ Grether, Daniel; Lineweaver, Charles H. (April 2006), "How Dry is the Brown Dwarf Desert? Quantifying the Relative Number of Planets, Brown Dwarfs, and Stellar Companions around Nearby Sun-like Stars", The Astrophysical Journal, 640 (2): 1051–1062, arXiv: astro-ph/0412356, Bibcode: 2006ApJ...640.1051G, doi: 10.1086/500161, S2CID 8563521.
External links
| Stars |
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Star clusters |
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| Nebulae |
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