Astronomy:54 Eridani

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Short description: Star in the constellation Eridanus
54 Eridani
Location of 54 Eridani (circled in red)
Observation data
Equinox J2000.0]] (ICRS)
Constellation Eridanus
Right ascension  04h 40m 26.51159s[1]
Declination −19° 40′ 17.3723″[1]
Apparent magnitude (V) 4.32[2]
Characteristics
Evolutionary stage asymptotic giant branch[3]
Spectral type M3/4 III[4]
U−B color index +1.80[5]
B−V color index 1.599±0.021[2]
Variable type SRb[6]
Astrometry
Radial velocity (Rv)−32.9±0.8[2] km/s
Proper motion (μ) RA: +29.13[7] mas/yr
Dec.: −96.42[7] mas/yr
Parallax (π)8.2063 ± 0.2709[1] mas
Distance400 ± 10 ly
(122 ± 4 pc)
Absolute magnitude (MV)−0.93[2]
Details
Mass3.95[8] M☉
Radius69+12
−6[1] R☉
Luminosity2,239[8] L☉
Surface gravity (log g)1.98[9] cgs
Temperature3,500[8] K
Metallicity [Fe/H]0.00[8] dex
Other designations
DM Eridani, BD−19°988, GC 5695, HD 29755, HIP 21763, HR 1496, SAO 149818, WDS J04404-1940[10]
Database references
SIMBADdata

54 Eridani is a suspected astrometric binary[11] star system located around 400 light years from the Sun in the barely equatorial-southern constellation of Eridanus. It is visible to the naked eye as a faint, reddish hued star with a baseline apparent visual magnitude of 4.32.[2] The object is moving closer to the Earth with a heliocentric radial velocity of −33 km/s.[2]

A light curve for DM Eridani, plotted from data published by Tabur et al. (2009)[12]

The variability of 54 Eridani was announced by Benjamin Apthorp Gould in his Uranometria Argentina, published in 1879.[13] But it was not given its variable star designation, DM Eridani, until nearly 100 years later, in 1973.[14] The visible component is an aging red giant star, currently on the asymptotic giant branch,[3] with a stellar classification of M3/4 III.[4] It is a semiregular variable star of subtype SRb, ranging in magnitude from 4.28 down to 4.36.[6] The star has pulsation periods of 18.8 and 45.5 days, each with an amplitude of 0.019 in magnitude.[12] With the hydrogen and helium at its core exhausted, the star has expanded to around 69 times the Sun's radius and it is radiating 1,021 times the luminosity of the Sun from its swollen photosphere at an effective temperature of 3,915 K.[1]

It was the second-brightest star in the obsolete constellation of Sceptrum Brandenburgicum after 53 Eridani.

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G.  Gaia DR2 record for this source at VizieR.
  2. ↑ 2.0 2.1 2.2 2.3 2.4 2.5 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A. 
  3. ↑ 3.0 3.1 Eggen, Olin J. (July 1992), "Asymptotic giant branch stars near the sun", Astronomical Journal 104 (1): 275–313, doi:10.1086/116239, Bibcode: 1992AJ....104..275E. 
  4. ↑ 4.0 4.1 Houk, Nancy; Smith-Moore, M. (1978), Michigan catalogue of two-dimensional spectral types for the HD stars, 4, Ann Arbor: Dept. of Astronomy, University of Michigan, Bibcode: 1988mcts.book.....H. 
  5. ↑ Mermilliod, J.-C. (1986). "Compilation of Eggen's UBV data, transformed to UBV (unpublished)". Catalogue of Eggen's UBV Data. Bibcode: 1986EgUBV........0M. 
  6. ↑ 6.0 6.1 Samus, N. N. et al. (2017), "General Catalogue of Variable Stars", Astronomy Reports, 5.1 61 (1): 80–88, doi:10.1134/S1063772917010085, Bibcode: 2017ARep...61...80S. 
  7. ↑ 7.0 7.1 Van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, doi:10.1051/0004-6361:20078357, Bibcode: 2007A&A...474..653V. 
  8. ↑ 8.0 8.1 8.2 8.3 Charbonnel, C.; Lagarde, N.; Jasniewicz, G.; North, P. L.; Shetrone, M.; Krugler Hollek, J.; Smith, V. V.; Smiljanic, R. et al. (2020). "Lithium in red giant stars: Constraining non-standard mixing with large surveys in the Gaia era". Astronomy and Astrophysics 633: A34. doi:10.1051/0004-6361/201936360. Bibcode: 2020A&A...633A..34C. 
  9. ↑ Khalatyan, A.; Anders, F.; Chiappini, C.; Queiroz, A. B. A.; Nepal, S.; Dal Ponte, M.; Jordi, C.; Guiglion, G. et al. (2024). "Transferring spectroscopic stellar labels to 217 million Gaia DR3 XP stars with SHBoost". Astronomy and Astrophysics 691: A98. doi:10.1051/0004-6361/202451427. Bibcode: 2024A&A...691A..98K. 
  10. ↑ "54 Eri". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=54+Eri. 
  11. ↑ 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, doi:10.1111/j.1365-2966.2008.13596.x, Bibcode: 2008MNRAS.389..869E. 
  12. ↑ 12.0 12.1 Tabur, V. et al. (December 2009), "Long-term photometry and periods for 261 nearby pulsating M giants", Monthly Notices of the Royal Astronomical Society 400 (4): 1945–1961, doi:10.1111/j.1365-2966.2009.15588.x, Bibcode: 2009MNRAS.400.1945T. 
  13. ↑ Gould, Benjamin Apthorp (1879). "Uranometria Argentina: Brightness and position of every fixed star, down to the seventh magnitude, within one hundred degrees of the South Pole; with atlas". Resultados del Observatorio Nacional Argentino 1: 162, 273. Bibcode: 1879RNAO....1....1G. 
  14. ↑ Kukarkin, B. V.; Kholopov, P. N.; Kukarkina, N. P.; Perova, N. B. (October 1973). "59th Name-List of Variable Stars". Information Bulletin on Variable Stars 834 (1–22): 1. Bibcode: 1973IBVS..834....1K. https://ibvs.konkoly.hu/pub/ibvs/0801/0834.pdf. Retrieved 8 December 2024. 



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