IM Pegasi

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IM Pegasi
Pegasus constellation map.svg
Red circle.svg
Location of IM Pegasi (circled)
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Pegasus
Right ascension 22h 53m 02.26608s [1]
Declination +16° 50′ 28.2969″ [1]
Apparent magnitude  (V)5.55 [2] (5.60 – 5.85 [3] )
Characteristics
Spectral type K2 III + dG [4]
Variable type RS CVn [3]
Astrometry
Radial velocity (Rv)−14.43 [5]  km/s
Proper motion (μ)RA: −20.73 [1]   mas/yr
Dec.: −27.75 [1]   mas/yr
Parallax (π)11.17 ± 0.33 [1]   mas
Distance 292 ± 9  ly
(90 ± 3  pc)
Orbit [2]
Period (P)24.64877±0.00003 d
Eccentricity (e)0.00
Inclination (i)65° ≤ i ≤ 80°°
Semi-amplitude (K1)
(primary)		34.29±0.04 km/s
Semi-amplitude(K2)
(secondary)		62.31±0.06 km/s
Details [4]
primary
Mass 1.8 ± 0.2  M☉
Radius 13.3 ± 0.6  R☉
Luminosity 54 ± 9  L☉
Temperature 4,550 ± 50  K
Rotation 24.4936 days
secondary
Mass 1.0 ± 0.07  M☉
Radius 1.00  R☉
Luminosity0.9 ± 0.3  L☉
Temperature 5,650 ± 200  K
Other designations
IM  Peg, HD  216489, HIP  112997, HR  8703, SAO  108231
Database references
SIMBAD data

IM Pegasi is a variable binary star system approximately 329 light-years away in the constellation of Pegasus. With an apparent magnitude of 5.7, it is visible to the naked eye. Increased public awareness of it is due to its use as the guide star for the Gravity Probe B general relativity experiment. It was chosen for this purpose because its microwave radio emissions are observable with a large radio telescope network on the ground in such a manner that its precise position can be related by interferometry to distant quasars. [6]

The two components of the binary system includes a K-type giant star and a G-type main sequence star. The primary star is estimated to be 1.8 times as massive and 13 times the diameter of the Sun. The secondary star is estimated to be similar to the Sun in size and mass. They orbit their common barycenter in a period precisely estimated to be 24.64877 days.

A visual band light curve for IM Pegasi, adapted from Eaton et al. (1983) IMPegLightCurve.png
A visual band light curve for IM Pegasi, adapted from Eaton et al. (1983)

The variability of IM Pegasi is due to the active chromosphere of the giant primary star, which causes brightness changes of a few tenths of a magnitude as it rotates.

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WR 12 is a spectroscopic binary in the constellation Vela. It is an eclipsing binary consisting of a Wolf-Rayet star and a luminous companion of unknown spectral type. The primary is one of the most luminous stars known.

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.
  2. 1 2 Berdyugina, S. V.; Ilyin, I.; Tuominen, I. (1999). "The long-period RS Canum Venaticorum binary IM Pegasi. I. Orbital and stellar parameters". Astronomy and Astrophysics. 347: 932. Bibcode:1999A&A...347..932B.
  3. 1 2 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.
  4. 1 2 Zellem, Robert; Guinan, Edward F.; Messina, Sergio; Lanza, Antonino F.; Wasatonic, Richard; McCook, George P. (2010). "Multiband Photometry of the Chromospherically Active & Spotted Binary System IM Peg-the Guide Star for the Gravity Probe B Mission". The Publications of the Astronomical Society of the Pacific. 122 (892): 670. Bibcode:2010PASP..122..670Z. doi: 10.1086/653711 .
  5. ↑ Karataș, Yüksel; Bilir, Selçuk; Eker, Zeki; Demircan, Osman; Liebert, James; Hawley, Suzanne L.; Fraser, Oliver J.; Covey, Kevin R.; Lowrance, Patrick; Kirkpatrick, J. Davy; Burgasser, Adam J. (2004). "Kinematics of chromospherically active binaries and evidence of an orbital period decrease in binary evolution". Monthly Notices of the Royal Astronomical Society. 349 (3): 1069–1092. arXiv: astro-ph/0404219 . Bibcode:2004MNRAS.349.1069K. doi:10.1111/j.1365-2966.2004.07588.x. S2CID   15290475.
  6. ↑ Shapiro, I. I.; Bartel, N.; Bietenholz, M. F.; Lebach, D. E.; Lestrade, J.-F.; Ransom, R. R.; Ratner, M. I. (2012). "VLBI for Gravity Probe B. I. Overview". The Astrophysical Journal Supplement. 201 (1): 1. arXiv: 1204.4630 . Bibcode:2012ApJS..201....1S. doi:10.1088/0067-0049/201/1/1. S2CID   51776288.
  7. ↑ Eaton, J. A.; Hall, D. S.; Henry, G. W.; Lovell, L. P.; Stephan, C. A.; Chambliss, C. R.; Detterline, P. K.; Landis, H. J.; Louth, H.; Renner, T. R.; Skillman, D. R. (January 1983). "Three Years of Photometry of IM-Pegasi = HR8703". Astrophysics and Space Science. 89 (1): 53–60. doi:10.1007/BF01008384 . Retrieved 12 February 2022.
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