KIC 9832227

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KIC 9832227
KIC 9832227

Observation data
Epoch J2000      Equinox J2000
Constellation Cygnus
Right ascension 19h 29m 15.948s[1]
Declination +46° 37′ 19.89″[1]
Apparent magnitude (V) 12.27 – 12.46[2]
Astrometry
Distance1843 ly
(565[3] pc)
Orbit[3]
Period (P)0.45796151 days
Semi-major axis (a)2.992 R
Inclination (i)53.2°
Periastron epoch (T)2455688.49913
Details[3]
A
Mass1.395 M
Radius1.581 R
Luminosity2.609 L
Surface gravity (log g)4.19 cgs
Temperature5800 K
Rotational velocity (v sin i)149.7 km/s
B
Mass0.318 M
Radius0.830 R
Luminosity0.789 L
Surface gravity (log g)4.10 cgs
Temperature5920 K
Rotational velocity (v sin i)84.7 km/s
Other designations
2MASS J19291594+4637198, KIC 9832227, ASAS J192916+4637.3, GSC 03543-01211
Database references
SIMBADdata
KICdata

KIC 9832227 is a contact binary star system[4] in the constellation Cygnus, located about 1,940 (± ~30) light-years away.[5] It is also identified as an eclipsing binary with an orbital period of almost 11 hours.[4] In 2017, the system was predicted to result in a merger in 2022.2 (± 0.6 years), producing a luminous red nova (LRN) reaching an apparent magnitude of 2.[5] The LRN should remain visible to the naked eye for roughly a month. The merger of the two stellar cores is predicted to give birth to a new, hotter, more massive main-sequence star.

The period of the variations in KIC 9832227 has been observed to be growing shorter since 2013. It is expected that the period will continue to get smaller at an ever-increasing rate, and end in the merging of the two cores. This will release a very large amount of energy, a process which occurred before in the system V1309 Scorpii, a nova which erupted in 2008, and was later found by a team led by Romuald Tylenda to have been the result of a stellar merger. However, astronomers in Tylenda's team have questioned the reliability of the KIC 9832227 prediction, because it is based on a model that may not be accurate enough to predict the eruption time so precisely.[6] The physical mechanism or mechanisms driving such stellar mergers is still not understood, and is the main focus of those researching KIC 9832227.

See also[edit]

References[edit]

  1. ^ a b Cutri, R. M. (2003). "2MASS All-Sky Catalog of Point Sources". VizieR On-line Data Catalog. 2246. Bibcode:2003yCat.2246....0C. 
  2. ^ "ASAS J192916+4637.3". AAVSO. Retrieved 7 January 2017. 
  3. ^ a b c Molnar, Lawrence A.; Van Noord, Daniel M.; Steenwyk, Steven D.; Spedden, Chris J.; Kinemuchi, Karen (2015). "A prediction of a luminous red nova eruption" (PDF). American Astronomical Society. 225 (225): 415.05. Bibcode:2015AAS...22541505M. Archived from the original (PDF) on 7 January 2017. 
  4. ^ a b Kinemuchi, Karen (2013-10-01). "To Pulsate or to Eclipse? Status of KIC 9832227 Variable Star". 1310: arXiv:1310.0544. arXiv:1310.0544Freely accessible. Bibcode:2013arXiv1310.0544K. 
  5. ^ a b Molnar, Lawrence A.; Van Noord, Daniel; Kinemuchi, Karen; Smolinski, Jason P.; Alexander, Cara E.; Kobulnicky, Henry A.; Cook, Evan M.; Jang, Byoungchan; Steenwyk, Steven D. (2017). "KIC 9832227: A red nova precursor". American Astronomical Society. 229: 417.04. Bibcode:2017AAS...22941704M. 
  6. ^ Carlisle, Camille (6 January 2017). "Paired Stars in Cygnus En Route to Merger". Sky and Telescope. Retrieved 12 January 2017. 

External links[edit]