  | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Perseus |
| Right ascension | 03h 05m 10.59385s [1] |
| Declination | +38° 50′ 24.9943″ [1] |
| Apparent magnitude (V) | +3.39 [2] |
| Characteristics | |
| Evolutionary stage | AGB [3] |
| Spectral type | M4 II [4] |
| U−B color index | +1.79 [2] |
| B−V color index | +1.65 [2] |
| Variable type | SRb [4] |
| Astrometry | |
| Radial velocity (Rv) | +29.10±0.30 [5] km/s |
| Proper motion (μ) |
RA: +129.22
[1]
mas/
yr Dec.: –105.70 [1] mas/ yr |
| Parallax (π) | 10.60 ± 0.25 mas [1] |
| Distance | 308 ± 7
ly (94 ± 2 pc) |
| Absolute magnitude (MV) | −1.7 [6] |
| Details [7] | |
| Mass | 1.9±0.7 M☉ |
| Radius | 143±12 R☉ |
| Luminosity | 2,692+192 −180 L☉ |
| Surface gravity (log g) | 0.37±0.15 cgs |
| Temperature | 3,479±125 K |
| Metallicity [Fe/H] | −0.15 dex |
| Rotational velocity (v sin i) | 11.2 [8] km/s |
| Age | 440 [9] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Rho Persei, Latinized from ρ Persei, is a star in the northern constellation of Perseus. It has the traditional name Gorgonea Tertia /ɡɔːrɡəˈniːə ˈtɜːrʃə/, [11] being the third member of the quartet called the Gorgonea in reference to the Gorgons from the legend of Perseus. [9] An apparent visual magnitude of +3.39 [2] makes it visible to the naked eye, but a challenge to view from a well-lit urban environment. Based upon parallax measurements, it is located at a distance of roughly 308 light-years (94 pc) from Earth. [1]
Rho Persei is a semiregular variable star, whose apparent magnitude varies between 3.3 and 4.0 [13] with periods of 50, 120 and 250 days. [6] The star has reached the asymptotic giant branch of its evolution. [3] It is a bright giant star with a stellar classification of M4 II. [4] The outer envelope has an effective temperature of 3,479 K, [7] giving it the red-orange hue of an M-type star. [14]
This star has a mass 1.9 times the mass of the Sun, while its radius has expanded to 143 times solar. It is radiating some 2,700 times the Sun's luminosity. [7] Rho Persei is losing mass at the rate of 1.2×10−8 solar masses per year, or the equivalent of the Sun's mass every 83 million years. [15] It is about 440 million years in age. [9]
Naming
In Chinese, 大陵 (Dà Líng), meaning Mausoleum, refers to an asterism consisting of ρ Persei, 9 Persei, τ Persei, ι Persei, κ Persei, β Persei, 16 Persei and 12 Persei. Consequently, the Chinese name for ρ Persei itself is 大陵六 (Dà Líng liù, English: the Sixth Star of Mausoleum.). [16]
References
- ^ a b c d e f van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv: 0708.1752, Bibcode: 2007A&A...474..653V, doi: 10.1051/0004-6361:20078357, S2CID 18759600
- ^ a b c d Nicolet, B. (1978), "Photoelectric photometric Catalogue of homogeneous measurements in the UBV System", Astronomy and Astrophysics Supplement Series, 34: 1–49, Bibcode: 1978A&AS...34....1N
- ^ a b Eggen, Olin J. (July 1992), "Asymptotic giant branch stars near the sun", Astronomical Journal, 104 (1): 275–313, Bibcode: 1992AJ....104..275E, doi: 10.1086/116239
- ^ a b c Ragland, S.; et al. (November 2006), "First Surface-resolved Results with the Infrared Optical Telescope Array Imaging Interferometer: Detection of Asymmetries in Asymptotic Giant Branch Stars", The Astrophysical Journal, 652 (1): 650–660, arXiv: astro-ph/0607156, Bibcode: 2006ApJ...652..650R, doi: 10.1086/507453, S2CID 30825403
- ^ Famaey, B.; et al. (May 2009), "Spectroscopic binaries among Hipparcos M giants. I. Data, orbits, and intrinsic variations", Astronomy and Astrophysics, 498 (2): 627–640, arXiv: 0901.0934, Bibcode: 2009A&A...498..627F, doi: 10.1051/0004-6361/200810698, S2CID 18739721
- ^ a b Yeşilyaprak, C.; Aslan, Z. (December 2004), "Period-luminosity relation for M-type semiregular variables from Hipparcos parallaxes", Monthly Notices of the Royal Astronomical Society, 355 (2): 601–607, Bibcode: 2004MNRAS.355..601Y, doi: 10.1111/j.1365-2966.2004.08344.x
- ^ a b c Kallinger, T.; et al. (April 2019), "Stellar masses from granulation and oscillations of 23 bright red giants observed by BRITE-Constellation", Astronomy & Astrophysics, 624: 17, arXiv: 1902.07531, Bibcode: 2019A&A...624A..35K, doi: 10.1051/0004-6361/201834514, S2CID 102486794, A35.
- ^ Massarotti, Alessandro; et al. (January 2008), "Rotational and Radial Velocities for a Sample of 761 HIPPARCOS Giants and the Role of Binarity", The Astronomical Journal, 135 (1): 209–231, Bibcode: 2008AJ....135..209M, doi: 10.1088/0004-6256/135/1/209
- ^ a b c Kaler, James B., "GORGONEA TERTIA (Rho Persei)", Stars, University of Illinois, retrieved 2012-01-25
- ^ "rho Per -- Semi-regular pulsating Star", SIMBAD, Centre de Données astronomiques de Strasbourg, retrieved 2012-01-24
- ^ Allen, Richard Hinckley (1899), "Star-names and their meanings", New York, G. E. Stechert: 334, Bibcode: 1899sntm.book.....A
- ^ Enhanced LCG, AAVSO, retrieved 21 September 2022.
- ^ Kukarkin, B. V.; et al. (1971), General Catalogue of Variable Stars (3rd ed.), Bibcode: 1971GCVS3.C......0K
- ^ "The Colour of Stars", Australia Telescope, Outreach and Education, Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, archived from the original on 2013-12-03, retrieved 2012-01-16
- ^ Cox, Arthur N.; Becker, Stephen A.; Pesnell, W. Dean (2000), "Chapter 20. Theoretical Stellar Evolution" (PDF), Allen's astrophysical quantities (4th ed.), New York: Springer, p. 516, ISBN 0-387-98746-0, archived from the original (PDF) on 2016-03-04, retrieved 2012-01-25 See table 20.5
- ^ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 11 日
External links
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| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Perseus |
| Right ascension | 03h 05m 10.59385s [1] |
| Declination | +38° 50′ 24.9943″ [1] |
| Apparent magnitude (V) | +3.39 [2] |
| Characteristics | |
| Evolutionary stage | AGB [3] |
| Spectral type | M4 II [4] |
| U−B color index | +1.79 [2] |
| B−V color index | +1.65 [2] |
| Variable type | SRb [4] |
| Astrometry | |
| Radial velocity (Rv) | +29.10±0.30 [5] km/s |
| Proper motion (μ) |
RA: +129.22
[1]
mas/
yr Dec.: –105.70 [1] mas/ yr |
| Parallax (π) | 10.60 ± 0.25 mas [1] |
| Distance | 308 ± 7
ly (94 ± 2 pc) |
| Absolute magnitude (MV) | −1.7 [6] |
| Details [7] | |
| Mass | 1.9±0.7 M☉ |
| Radius | 143±12 R☉ |
| Luminosity | 2,692+192 −180 L☉ |
| Surface gravity (log g) | 0.37±0.15 cgs |
| Temperature | 3,479±125 K |
| Metallicity [Fe/H] | −0.15 dex |
| Rotational velocity (v sin i) | 11.2 [8] km/s |
| Age | 440 [9] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Rho Persei, Latinized from ρ Persei, is a star in the northern constellation of Perseus. It has the traditional name Gorgonea Tertia /ɡɔːrɡəˈniːə ˈtɜːrʃə/, [11] being the third member of the quartet called the Gorgonea in reference to the Gorgons from the legend of Perseus. [9] An apparent visual magnitude of +3.39 [2] makes it visible to the naked eye, but a challenge to view from a well-lit urban environment. Based upon parallax measurements, it is located at a distance of roughly 308 light-years (94 pc) from Earth. [1]
Rho Persei is a semiregular variable star, whose apparent magnitude varies between 3.3 and 4.0 [13] with periods of 50, 120 and 250 days. [6] The star has reached the asymptotic giant branch of its evolution. [3] It is a bright giant star with a stellar classification of M4 II. [4] The outer envelope has an effective temperature of 3,479 K, [7] giving it the red-orange hue of an M-type star. [14]
This star has a mass 1.9 times the mass of the Sun, while its radius has expanded to 143 times solar. It is radiating some 2,700 times the Sun's luminosity. [7] Rho Persei is losing mass at the rate of 1.2×10−8 solar masses per year, or the equivalent of the Sun's mass every 83 million years. [15] It is about 440 million years in age. [9]
Naming
In Chinese, 大陵 (Dà Líng), meaning Mausoleum, refers to an asterism consisting of ρ Persei, 9 Persei, τ Persei, ι Persei, κ Persei, β Persei, 16 Persei and 12 Persei. Consequently, the Chinese name for ρ Persei itself is 大陵六 (Dà Líng liù, English: the Sixth Star of Mausoleum.). [16]
References
- ^ a b c d e f van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv: 0708.1752, Bibcode: 2007A&A...474..653V, doi: 10.1051/0004-6361:20078357, S2CID 18759600
- ^ a b c d Nicolet, B. (1978), "Photoelectric photometric Catalogue of homogeneous measurements in the UBV System", Astronomy and Astrophysics Supplement Series, 34: 1–49, Bibcode: 1978A&AS...34....1N
- ^ a b Eggen, Olin J. (July 1992), "Asymptotic giant branch stars near the sun", Astronomical Journal, 104 (1): 275–313, Bibcode: 1992AJ....104..275E, doi: 10.1086/116239
- ^ a b c Ragland, S.; et al. (November 2006), "First Surface-resolved Results with the Infrared Optical Telescope Array Imaging Interferometer: Detection of Asymmetries in Asymptotic Giant Branch Stars", The Astrophysical Journal, 652 (1): 650–660, arXiv: astro-ph/0607156, Bibcode: 2006ApJ...652..650R, doi: 10.1086/507453, S2CID 30825403
- ^ Famaey, B.; et al. (May 2009), "Spectroscopic binaries among Hipparcos M giants. I. Data, orbits, and intrinsic variations", Astronomy and Astrophysics, 498 (2): 627–640, arXiv: 0901.0934, Bibcode: 2009A&A...498..627F, doi: 10.1051/0004-6361/200810698, S2CID 18739721
- ^ a b Yeşilyaprak, C.; Aslan, Z. (December 2004), "Period-luminosity relation for M-type semiregular variables from Hipparcos parallaxes", Monthly Notices of the Royal Astronomical Society, 355 (2): 601–607, Bibcode: 2004MNRAS.355..601Y, doi: 10.1111/j.1365-2966.2004.08344.x
- ^ a b c Kallinger, T.; et al. (April 2019), "Stellar masses from granulation and oscillations of 23 bright red giants observed by BRITE-Constellation", Astronomy & Astrophysics, 624: 17, arXiv: 1902.07531, Bibcode: 2019A&A...624A..35K, doi: 10.1051/0004-6361/201834514, S2CID 102486794, A35.
- ^ Massarotti, Alessandro; et al. (January 2008), "Rotational and Radial Velocities for a Sample of 761 HIPPARCOS Giants and the Role of Binarity", The Astronomical Journal, 135 (1): 209–231, Bibcode: 2008AJ....135..209M, doi: 10.1088/0004-6256/135/1/209
- ^ a b c Kaler, James B., "GORGONEA TERTIA (Rho Persei)", Stars, University of Illinois, retrieved 2012-01-25
- ^ "rho Per -- Semi-regular pulsating Star", SIMBAD, Centre de Données astronomiques de Strasbourg, retrieved 2012-01-24
- ^ Allen, Richard Hinckley (1899), "Star-names and their meanings", New York, G. E. Stechert: 334, Bibcode: 1899sntm.book.....A
- ^ Enhanced LCG, AAVSO, retrieved 21 September 2022.
- ^ Kukarkin, B. V.; et al. (1971), General Catalogue of Variable Stars (3rd ed.), Bibcode: 1971GCVS3.C......0K
- ^ "The Colour of Stars", Australia Telescope, Outreach and Education, Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, archived from the original on 2013-12-03, retrieved 2012-01-16
- ^ Cox, Arthur N.; Becker, Stephen A.; Pesnell, W. Dean (2000), "Chapter 20. Theoretical Stellar Evolution" (PDF), Allen's astrophysical quantities (4th ed.), New York: Springer, p. 516, ISBN 0-387-98746-0, archived from the original (PDF) on 2016-03-04, retrieved 2012-01-25 See table 20.5
- ^ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 11 日
External links
| Stars |
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|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
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Star clusters |
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| Nebulae |
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| Galaxies |
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