T Coronae Borealis
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
Constellation | Corona Borealis |
Right ascension | 15h 59m 30.1622s[1] |
Declination | 25° 55′ 12.613″[1] |
Apparent magnitude (V) | 2.0–10.8[2] |
| Characteristics | |
Evolutionary stage | Red giant + white dwarf |
Spectral type | M3III+p[3] |
Variable type | recurrent nova[2] |
| Astrometry | |
| Radial velocity (Rv) | −27.79[4] km/s |
| Parallax (π) | 1.33 ± 0.57[1] mas |
| Distance | approx. 2,000 ly (approx. 800 pc) |
| Orbit | |
| Period (P) | 228[5]yr |
| Eccentricity (e) | 0.0[5] |
| Inclination (i) | 67[6]° |
| Details | |
| Giant | |
| Mass | 0.8[7] M☉ |
| Surface gravity (log g) | 2.0[8] cgs |
| Temperature | 3,600[8] K |
| White dwarf | |
| Mass | 1.2[7] M☉ |
| Luminosity | 40[7] L☉ |
| Other designations | |
BD+26° 2765, HD 143454, HIP 78322, SAO 84129, 2MASS J15593015+2555126 | |
| Database references | |
| SIMBAD | data |
T Coronae Borealis (T CrB), is a recurring nova in the constellation Corona Borealis. It was first discovered in outburst in 1866 by John Birmingham,[9] although it had been observed earlier as a 10th magnitude star.[10]
Contents
1 Description
2 2016-present Activity
3 References
4 Further reading
5 External links
Description
AAVSO light curve of recurrent nova T CrB from 1 Jan 2008 to 17 Nov 2010, showing the pulsations of the red giant primary. Up is brighter and down is fainter. Day numbers are Julian day.
T CrB normally has an magnitude of about 10, which is near the limit of typical binoculars. It has been seen to outburst twice, reaching magnitude 2.0 on May 12, 1866 and magnitude 3.0 on February 9, 1946.[11] Though a more recent paper shows the 1866 outburst with a possible peak range of magnitude 2.5 ± 0.5.[12] Even when at peak magnitude of 2.5, this recurrent nova is dimmer than about 120 stars in the night sky.[13] It is sometimes nicknamed the Blaze Star,[14]
2016-present Activity
On 20 April 2016, the Sky and Telescope newsletter reported a recent sustained brightening since February 2015 from magnitude 10.5 to about 9.2. A similar event was reported in 1938, shortly before the 1946 outburst.[15] As of June 2018, the star has dimmed slightly but still remains at an unusually high level of activity.
References
^ abc Gaia Collaboration; et al. (November 2016). "Gaia Data Release 1. Summary of the astrometric, photometric, and survey properties". Astronomy & Astrophysics. 595: 23. arXiv:1609.04172. Bibcode:2016A&A...595A...2G. doi:10.1051/0004-6361/201629512. A2..mw-parser-output cite.citation{font-style:inherit}.mw-parser-output q{quotes:"""""""'""'"}.mw-parser-output code.cs1-code{color:inherit;background:inherit;border:inherit;padding:inherit}.mw-parser-output .cs1-lock-free a{background:url("//upload.wikimedia.org/wikipedia/commons/thumb/6/65/Lock-green.svg/9px-Lock-green.svg.png")no-repeat;background-position:right .1em center}.mw-parser-output .cs1-lock-limited a,.mw-parser-output .cs1-lock-registration a{background:url("//upload.wikimedia.org/wikipedia/commons/thumb/d/d6/Lock-gray-alt-2.svg/9px-Lock-gray-alt-2.svg.png")no-repeat;background-position:right .1em center}.mw-parser-output .cs1-lock-subscription a{background:url("//upload.wikimedia.org/wikipedia/commons/thumb/a/aa/Lock-red-alt-2.svg/9px-Lock-red-alt-2.svg.png")no-repeat;background-position:right .1em center}.mw-parser-output .cs1-subscription,.mw-parser-output .cs1-registration{color:#555}.mw-parser-output .cs1-subscription span,.mw-parser-output .cs1-registration span{border-bottom:1px dotted;cursor:help}.mw-parser-output .cs1-hidden-error{display:none;font-size:100%}.mw-parser-output .cs1-visible-error{font-size:100%}.mw-parser-output .cs1-subscription,.mw-parser-output .cs1-registration,.mw-parser-output .cs1-format{font-size:95%}.mw-parser-output .cs1-kern-left,.mw-parser-output .cs1-kern-wl-left{padding-left:0.2em}.mw-parser-output .cs1-kern-right,.mw-parser-output .cs1-kern-wl-right{padding-right:0.2em}
^ ab 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.
^ Pourbaix, D.; Tokovinin, A. A.; Batten, A. H.; Fekel, F. C.; Hartkopf, W. I.; Levato, H.; Morrell, N. I.; Torres, G.; Udry, S. (2004). "SB9: The ninth catalogue of spectroscopic binary orbits". Astronomy and Astrophysics. 424 (2): 727. arXiv:astro-ph/0406573. Bibcode:2004A&A...424..727P. doi:10.1051/0004-6361:20041213.
^ ab Fekel, Francis C.; Joyce, Richard R.; Hinkle, Kenneth H.; Skrutskie, Michael F. (2000). "Infrared Spectroscopy of Symbiotic Stars. I. Orbits for Well-Known S-Type Systems". The Astronomical Journal. 119 (3): 1375. Bibcode:2000AJ....119.1375F. doi:10.1086/301260.
^ Stanishev, V.; Zamanov, R.; Tomov, N.; Marziani, P. (2004). "Hα variability of the recurrent nova T Coronae Borealis". Astronomy and Astrophysics. 415 (2): 609. arXiv:astro-ph/0311309. Bibcode:2004A&A...415..609S. doi:10.1051/0004-6361:20034623.
^ abc Iłkiewicz, Krystian; Mikołajewska, Joanna; Stoyanov, Kiril; Manousakis, Antonios; Miszalski, Brent (2016). "Active phases and flickering of a symbiotic recurrent nova T CrB". Monthly Notices of the Royal Astronomical Society. 462 (3): 2695. arXiv:1607.06804. Bibcode:2016MNRAS.462.2695I. doi:10.1093/mnras/stw1837.
^ ab Wallerstein, George; Harrison, Tanya; Munari, Ulisse; Vanture, Andrew (2008). "The Metallicity and Lithium Abundances of the Recurring Novae T CrB and RS Oph". Publications of the Astronomical Society of the Pacific. 120 (867): 492. Bibcode:2008PASP..120..492W. doi:10.1086/587965.
^ Pettit, Edison (1946). "The Light-Curves of T Coronae Borealis". Publications of the Astronomical Society of the Pacific. 58: 153. Bibcode:1946PASP...58..153P. doi:10.1086/125797.
^ Barnard, E. E. (1907). "Nova T Coronae of 1866". Astrophysical Journal. 25: 279. Bibcode:1907ApJ....25..279B. doi:10.1086/141446.
^ Sanford, Roscoe F. (1949). "High-Dispersion Spectrograms of T Coronae Borealis". Astrophysical Journal. 109: 81. Bibcode:1949ApJ...109...81S. doi:10.1086/145106.
^ Schaefer, Bradley E. (2009). "Comprehensive Photometric Histories of All Known Galactic Recurrent Novae". The Astrophysical Journal Supplement Series. 187 (2): 275–373. arXiv:0912.4426. Bibcode:2010ApJS..187..275S. doi:10.1088/0067-0049/187/2/275.
^ "Vmag<2.5". SIMBAD Astronomical Database. Retrieved 2010-06-25.
^ A Digital Spectral Classification Atlas, R. O. Gray, 34. Unusual Stellar Spectra III: two emission-line stars
^ "Is T CrB About to Blow its Top?". Sky and Telescope newsletter. Retrieved 2017-08-06.
Further reading
Wallerstein, George; Tanya Harrison; Ulisse Munari; Andrew Vanture (11 May 2008). "The Metallicity and Lithium Abundances of the Recurring Novae T CrB and RS Oph". Publications of the Astronomical Society of the Pacific. 120 (867): 492–497. Bibcode:2008PASP..120..492W. doi:10.1086/587965.
R and T Coronae Borealis: Two Stellar Opposites at Sky & Telescope
External links
- http://www.daviddarling.info/encyclopedia/B/Blaze_Star.html
- AAVSO: Quick Look View of AAVSO Observations (get recent magnitude estimates for T CrB)
