48 Persei

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48 Persei
Perseus constellation map.svg
Red circle.svg
Location of 48 Persei (circled)
Observation data
Epoch J2000       Equinox J2000
Constellation Perseus
Right ascension 04h 08m 39.69216s [1]
Declination 47° 42′ 45.0429″ [1]
Apparent magnitude  (V)4.03 [2]
Characteristics
Evolutionary stage Main sequence
Spectral type B3Ve [3]
U−B color index -0.55 [2]
B−V color index -0.03 [2]
Variable type γ Cas [4]
Astrometry
Radial velocity (Rv)+0.80 [5]  km/s
Proper motion (μ)RA: +21.73 [1]   mas/yr
Dec.: -33.61 [1]   mas/yr
Parallax (π)6.84 ± 0.16  mas [1]
Distance 480 ± 10  ly
(146 ± 3  pc)
Absolute magnitude  (MV)-1.86 [6]
Details
Mass 7.5 [7]   M☉
Luminosity 600 [6]   L☉
Surface gravity (log g)3.86 [8]   cgs
Temperature 17,490 [8]   K
Metallicity [Fe/H]-0.04 [9]   dex
Rotational velocity (v sin i)197 [8]  km/s
Other designations
c Persei, MX Persei, BD+47°939, FK5  152, GC  4967, HIP  19343, HR  1273, HD  25940, SAO  39336
Database references
SIMBAD data

48 Persei (also known as c Persei, 48 Per, HR 1273, HIP 19343, or HD 25940) is a Be star in the constellation Perseus, approximately the 500th brightest of the visible stars in apparent magnitude. [10] It is "well known for its complex spectrum and for its light and velocity variations". [11] The name "48 Persei" is a Flamsteed designation given to it by John Flamsteed in his catalogue, published in 1712. [12]

A light curve for MX Persei, plotted from Hipparcos data MXPerLightCurve.png
A light curve for MX Persei, plotted from Hipparcos data

48 Persei is classified as a Gamma Cassiopeiae variable, and it has been given the variable star designation MX Persei. The star's brightness varies by 0.09 magnitudes in visible light. [14] Koen and Eyer examined the Hipparcos data for this star, and found it varied with a period of 5.0569 days. [15]

As a Be star, it is hot and blue, spinning so rapidly that it forms an unstable equatorial disk of matter surrounding it. Its mass has been estimated as seven times that of the Sun, and its estimated age of 40 million years makes it much younger than the Sun. In another few million years it will likely cease hydrogen fusion, expand, and brighten as it becomes a red giant. [16]

A 1989 study proposed 48 Persei to be a single-lined spectroscopic binary with a period of 16.6 days, but subsequent studies, including close imaging surveys, have not confirmed this result. Hutter et al. (2021) consider it to be a single star. [17]

Related Research Articles

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<span class="mw-page-title-main">10 Leonis Minoris</span> Star in the constellation Leo Minor

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<span class="mw-page-title-main">4 Persei</span> Star in the constellation Perseus

4 Persei is a single star in the northern constellation of Perseus, located around 670 light years away from the Sun. It is visible to the naked eye as a faint, blue-white hued star with an apparent visual magnitude of 5.04 The Bayer designation for this star is g Persei; 4 Persei is the Flamsteed designation. This object has a peculiar velocity of 26.3 km/s and may be a runaway star.

<span class="mw-page-title-main">29 Persei</span> Star in the constellation Perseus

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<span class="mw-page-title-main">9 Persei</span> Blue supergiant star in the constellation Perseus

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<span class="mw-page-title-main">42 Persei</span> Binary star system in the constellation Perseus

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<span class="mw-page-title-main">31 Persei</span> Star in the constellation Perseus

31 Persei is a single star in the northern constellation of Perseus. It is visible to the naked eye as a dim, blue-white hued point of light with an apparent visual magnitude of 5.05. This star is located around 172 parsecs (560 ly) away from the Sun, and it is drifting closer with a radial velocity of −1.6 km/s. It is likely a member of the Alpha Persei Cluster.

<span class="mw-page-title-main">21 Persei</span> Star in the constellation Perseus

21 Persei is a single, variable star in the northern constellation of Perseus, located about 331 light years away from the Sun. It is visible to the naked eye as a faint, white-hued star with an apparent visual magnitude of 5.10 km/s. The object is moving further from the Earth with a heliocentric radial velocity of +8.5 km/s. It has the variable star designation LT Persei; 21 Persei is the Flamsteed designation.

<span class="mw-page-title-main">V520 Persei</span> Star in the constellation Perseus

V520 Persei is a blue supergiant member of NGC 869, one of the Perseus Double Cluster open clusters. It is an irregular variable star. At a magnitude of 6.55, V520 Persei is the brightest member in either NGC 869 or NGC 884, although the brighter HD 13994 lies in the foreground along the same line of sight.

References

  1. 1 2 3 4 5 Van Leeuwen, F. (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. Vizier catalog entry
  2. 1 2 3 Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues. 2237. Bibcode:2002yCat.2237....0D.
  3. ↑ Hoffleit, D.; Warren, W. H. (1995). "VizieR Online Data Catalog: Bright Star Catalogue, 5th Revised Ed. (Hoffleit+, 1991)". VizieR On-line Data Catalog: V/50. Originally Published in: 1964BS....C......0H. 5050. Bibcode:1995yCat.5050....0H.
  4. ↑ Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1. Bibcode:2009yCat....102025S.
  5. ↑ Evans, D. S. (1967). "The Revision of the General Catalogue of Radial Velocities". Determination of Radial Velocities and Their Applications. 30: 57. Bibcode:1967IAUS...30...57E.
  6. 1 2 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331. arXiv: 1108.4971 . Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. S2CID   119257644. Vizier catalog entry
  7. ↑ Tetzlaff, N.; Neuhäuser, R.; Hohle, M. M. (2011). "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun". Monthly Notices of the Royal Astronomical Society. 410 (1): 190–200. arXiv: 1007.4883 . Bibcode:2011MNRAS.410..190T. doi: 10.1111/j.1365-2966.2010.17434.x . S2CID   118629873. Vizier catalog entry
  8. 1 2 3 Zorec, J.; Frémat, Y.; Domiciano De Souza, A.; Royer, F.; Cidale, L.; Hubert, A.-M.; Semaan, T.; Martayan, C.; Cochetti, Y. R.; Arias, M. L.; Aidelman, Y.; Stee, P. (2016). "Critical study of the distribution of rotational velocities of Be stars". Astronomy & Astrophysics. 595: A132. Bibcode:2016A&A...595A.132Z. doi: 10.1051/0004-6361/201628760 . hdl: 11336/37946 .
  9. ↑ Wu, Yue; Singh, H. P.; Prugniel, P.; Gupta, R.; Koleva, M. (2010). "Coudé-feed stellar spectral library – atmospheric parameters". Astronomy & Astrophysics. 525: A71. arXiv: 1009.1491 . Bibcode:2011A&A...525A..71W. doi:10.1051/0004-6361/201015014. S2CID   53480665.
  10. ↑ 48 Persei (HIP 19343), Ashland Astronomy Studio, archived from the original on 2013-01-02, retrieved 2012-12-28.
  11. ↑ Percy, J. R.; Lane, M. C. (May 1977), "Search for Beta Cephei stars. I - Photometric and spectroscopic studies of northern B-type stars", Astronomical Journal, 82: 353–359, Bibcode:1977AJ.....82..353P, doi:10.1086/112057 .
  12. ↑ Baily, Francis, ed. (1835), An account of the Revd. John Flamsteed, the first astronomer-royal: compiled from his own manuscripts, and other authentic documents, never before published. To which is added his British catalogue of stars, cor. and enl., Lords Commissioners of the Admiralty, p. 425.
  13. ↑ "/ftp/cats/more/HIP/cdroms/cats". Centre de Données astronomiques de Strasbourg. Strasbourg astronomical Data Center. Retrieved 15 October 2022.
  14. ↑ "MX Per". The International Variable Star Index. AAVSO. Retrieved 30 November 2022.
  15. ↑ Koen, Chris; Eyer, Laurent (March 2002). "New periodic variables from the Hipparcos epoch photometry". Monthly Notices of the Royal Astronomical Society. 331 (1): 45–59. arXiv: astro-ph/0112194 . Bibcode:2002MNRAS.331...45K. doi: 10.1046/j.1365-8711.2002.05150.x . S2CID   10505995.
  16. ↑ Kaler, Jim (2009-01-16), "48 Per (48 Persei)", STARS, University of Illinois , retrieved 2012-12-28.
  17. ↑ Hutter, D. J.; Tycner, C.; Zavala, R. T.; Benson, J. A.; Hummel, C. A.; Zirm, H. (2021). "Surveying the Bright Stars by Optical Interferometry. III. A Magnitude-limited Multiplicity Survey of Classical Be Stars". The Astrophysical Journal Supplement Series. 257 (2): 69. arXiv: 2109.06839 . Bibcode:2021ApJS..257...69H. doi: 10.3847/1538-4365/ac23cb . S2CID   237503492.

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