1 Persei

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1 Persei
Perseus constellation map.svg
Red circle.svg
Location of 1 Persei (circled)
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Perseus
Right ascension 01h 51m 59.32008s [1]
Declination +55° 08′ 50.5837″ [1]
Apparent magnitude  (V)5.49 - 5.74 - 5.85 [2]
Characteristics
Spectral type B1.5V [2]
Variable type eclipsing binary [3]
Astrometry
Proper motion (μ)RA: 12.716(74) [1]   mas/yr
Dec.: −8.410(79) [1]   mas/yr
Parallax (π)2.6944 ± 0.0888  mas [1]
Distance 1,210 ± 40  ly
(370 ± 10  pc)
Absolute magnitude  (MV)−1.37/−1.77 [4]
Orbit [4]
Primary1 Persei A
Companion1 Persei B
Period (P)25.935951±0.000003 d
Eccentricity (e)0.3768±0.0014
Inclination (i)88.048±0.002°
Periastron epoch (T)2443563.466±0.005  HJD
Argument of periastron (ω)
(secondary)		109.83±0.10°
Semi-amplitude (K1)
(primary)		97.4±0.1 km/s
Semi-amplitude (K2)
(secondary)		91.2±0.1 km/s
Details [4]
Primary
Mass 6.95  M☉
Radius 3.29  R☉
Luminosity 2,188  L☉
Surface gravity (log g)4.25  cgs
Temperature 21,500  K
Rotation 1.45 days
Rotational velocity (v sin i)115 km/s
Secondary
Mass 7.42  M☉
Radius 3.86  R☉
Luminosity3,311  L☉
Surface gravity (log g)4.14  cgs
Temperature 22,000  K
Rotation 1.40 days
Rotational velocity (v sin i)140 km/s
Other designations
V436 Persei, BD+54 396, HD  11241, HIP  8704, HR  533, SAO  22690
Database references
SIMBAD data

1 Persei (1 Per) is an eclipsing binary [3] star in the constellation Perseus. Its uneclipsed apparent magnitude is 5.49. The binary star consists of two B2 type main-sequence stars in a 25.9 day eccentric orbit. [5] The stars are surrounded by a faint cloud of gas visible in mid-infrared, although whether they are the origin of the gas or simply passing through it is unclear.

Observational history

A visual band light curve for V436 Persei, adapted from Janik et al. (2003) V436PerLightCurve.png
A visual band light curve for V436 Persei, adapted from Janik et al. (2003)

The possible eclipsing binary nature of 1 Persei was first noticed by Donald Kurtz in 1977 when it was used as a comparison star to test for photometric variability of HD 11408. [6] In 1979 French amateur observers succeeded in determining an orbital period of 25.9 days. [7] During the primary eclipse, the brightness drops to magnitude 5.85. In the secondary eclipses, the brightness drops to magnitude 5.74. The eclipses each last for approximately 25 hours. [2]

Related Research Articles

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Gamma Persei Binary star system in the constellation Perseus

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Delta Sagittae Star in the constellation Sagitta

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Tau Persei Star in the constellation Perseus

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42 Persei Star in the constellation Perseus

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ZZ Boötis

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HR 7484 Star in the constellation Cygnus

HR 7484 is a binary star system in the northern constellation of Cygnus. It is dimly visible to the naked eye under good viewing conditions, having an apparent visual magnitude of 5.89. Based upon an annual parallax shift of 24.71, it is located 132 light years away. The system is moving closer with a heliocentric radial velocity of −14 km/s.

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WR 9 Star in the constellation Puppis

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V346 Centauri

V346 Centauri is a variable star in the constellation Centaurus. An Algol-type eclipsing binary, its apparent magnitude has a maximum of 8.50, dropping to 8.77 during primary eclipse and to 8.72 during secondary eclipse, the latter being a total eclipse. From parallax measurements by the Gaia spacecraft, the system is located at a distance of about 2300 parsecs (7400 light-years), which is consistent with earlier estimates, based on its luminosity, of 2380 parsecs. The system is a confirmed member of the open cluster Stock 14, which contains many other young OB stars.

References

  1. 1 2 3 4 5 Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics . 649: A1. arXiv: 2012.01533 . Bibcode:2021A&A...649A...1G. doi: 10.1051/0004-6361/202039657 . S2CID   227254300. (Erratum:  doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  2. 1 2 3 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.
  3. 1 2 North, P.; et al. (1981). "1 Per: a new eclipsing binary with a long period and an elliptical orbit" (PDF). Information Bulletin on Variable Stars. 2036: 1. Bibcode:1981IBVS.2036....1N.
  4. 1 2 3 4 Janík, J.; et al. (2003). "Search for forced oscillations in binaries. IV. The eclipsing binary V436 Per revisited". Astronomy and Astrophysics. 408 (2): 611–619. Bibcode:2003A&A...408..611J. doi: 10.1051/0004-6361:20030960 .
  5. ↑ Harmanec, P.; et al. (1997). "Search for forced oscillations in binaries. I. The eclipsing and spectroscopic binary V436 Persei = 1 Persei". Astronomy and Astrophysics. 319 (2): 867–880. Bibcode:1997A&A...319..867H.
  6. ↑ Kurtz, D. W. (1977). "The photometric variability of 1 Per". Publications of the Astronomical Society of the Pacific. 89: 939–940. Bibcode:1977PASP...89..939K. doi: 10.1086/130251 .
  7. ↑ Figer, Alain; Maurin, Luc (1979). "1 Persei, a low amplitude eclipsing binary, has a period of 25.939 days and an elliptical orbit". GEOS Circular on Eclipsing Binaries. 2 (EB 2). Bibcode:1979GEOCE...2.....F.
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