Upsilon4 Eridani

From Wikipedia, the free encyclopedia
Jump to: navigation, search
Upsilon4 Eridani
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Eridanus
Right ascension 04h 17m 53.66241s[1]
Declination −33° 47′ 54.0569″[1]
Apparent magnitude (V) 3.56[2]
Characteristics
Spectral type B8V + B9.5V[3]
U−B color index −0.36[2]
B−V color index −0.12[2]
Astrometry
Radial velocity (Rv) +17.6[4] km/s
Proper motion (μ) RA: +62.52[1] mas/yr
Dec.: −7.24[1] mas/yr
Parallax (π) 18.33 ± 0.15[1] mas
Distance 178 ± 1 ly
(54.6 ± 0.4 pc)
Absolute magnitude (MV) −0.20[5]
Orbit[6]
Period (P) 5.0103250±0.0000008 d
Semi-major axis (a) 1.902±0.006 mas
Eccentricity (e) 0
Inclination (i) 146.2±0.1°
Periastron epoch (T) 2454407.7214 ± 0.002 JD
Semi-amplitude (K1)
(primary)
62.68±0.17[7] km/s
Semi-amplitude (K2)
(secondary)
64.70±0.15[7] km/s
Details[6]
υ4 Eri A
Mass 3.17±0.07 M
Radius 2.32±0.18 R
Luminosity 100.6±4.3 L
Surface gravity (log g) 4.21±0.07 cgs
Temperature 12,930±440[8] K
Rotational velocity (v sin i) 19[8] km/s
Age 146[8] Myr
υ4 Eri B
Mass 3.07±0.07 M
Radius 2.32±0.18 R
Luminosity 87.4±3.3 L
Surface gravity (log g) 4.21±0.07 cgs
Temperature 12,250 K
Other designations
υ4 Eri, 41 Eridani, CD−34° 1614, HD 27376, HIP 20042, HR 1347, SAO 194902.[9]
Database references
SIMBAD data

Upsilon4 Eridani is a close binary star system in the constellation Eridanus. It is visible to the naked eye with an apparent visual magnitude of 3.56.[2] Based upon parallax measurements, the pair are located around 54.6 parsecs (178 ly) from the Sun.[1]

This is a double-lined spectroscopic binary star system,[10] which means that the Doppler-shifted spectral lines of both components can be distinguished. The pair have a circular orbit with a period of five days. The system is composed of two B-type main-sequence stars: one has a stellar classification of B8V and the other B9.5V.[3] Both stars show HgMn peculiarities in their spectrum,[7] and their properties are nearly identical.[6] The spin rate of the two stars is synchronized to their orbital period.[6] It is possible that a nearby K-type star is also related.[3]

References[edit]

  1. ^ a b c d e f van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752Freely accessible, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357. 
  2. ^ a b c d Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV data, SIMBAD, Bibcode:1986EgUBV........0M. 
  3. ^ a b c 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:0806.2878Freely accessible, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x. 
  4. ^ Evans, D. S. (June 20–24, 1966), Batten, Alan Henry; Heard, John Frederick, eds., "The Revision of the General Catalogue of Radial Velocities", Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30, University of Toronto: International Astronomical Union, Bibcode:1967IAUS...30...57E. 
  5. ^ Hubrig, S.; et al. (June 2001), "Search for low-mass PMS companions around X-ray selected late B stars", Astronomy and Astrophysics, 372: 152−164, arXiv:astro-ph/0103201Freely accessible, Bibcode:2001A&A...372..152H, doi:10.1051/0004-6361:20010452. 
  6. ^ a b c d Hummel, Christian A.; et al. (March 2017), "The orbit of the mercury-manganese binary 41 Eridani", Astronomy & Astrophysics, 600 (L5): 6, arXiv:1703.07668Freely accessible, Bibcode:2016SPIE.9907E..0QH, doi:10.1117/12.2231859. 
  7. ^ a b c Hubrig, S.; et al. (November 2012), "Magnetic fields of HgMn stars", Astronomy & Astrophysics, 547: 24, arXiv:1208.2910Freely accessible, Bibcode:2012A&A...547A..90H, doi:10.1051/0004-6361/201219778, A90. 
  8. ^ a b c David, Trevor J.; Hillenbrand, Lynne A. (2015), "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets", The Astrophysical Journal, 804 (2): 146, arXiv:1501.03154Freely accessible, Bibcode:2015ApJ...804..146D, doi:10.1088/0004-637X/804/2/146. 
  9. ^ "* ups04 Eri -- Spectroscopic binary". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2016-10-13. 
  10. ^ Chini, R.; et al. (2012), "A spectroscopic survey on the multiplicity of high-mass stars", Monthly Notices of the Royal Astronomical Society, 424 (3): 1925, arXiv:1205.5238Freely accessible, Bibcode:2012MNRAS.424.1925C, doi:10.1111/j.1365-2966.2012.21317.x.