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Sigma Coronae Borealis

A light curve for TZ Coronae Borealis, plotted from TESS data
Observation data Epoch J2000      Equinox J2000
Constellation	Corona Borealis
σ CrB A (σ)
Right ascension	16 14 40.854
Declination	+33° 51′ 31.02″
Apparent magnitude (V)	5.55
σ CrB B (σ)
Right ascension	16 14 40.394
Declination	+33° 51′ 27.05″
Apparent magnitude (V)	6.419
σ CrB C
Right ascension	16 13 56.26666
Declination	+33° 46′ 24.2953″
Apparent magnitude (V)	12.229
Characteristics
σ CrB
Spectral type	F6V (A) + G1V (B)
U−B color index	+0.045
B−V color index	+0.599
Variable type	RS CVn
σ CrB C
Spectral type	M2.5V
Astrometry
σ CrB A
Radial velocity (Rv)	−12.30 ± 0.06 km/s
Proper motion (μ)	RA: −268.325 mas/yr Dec.: −86.925 mas/yr
Parallax (π)	44.1346 ± 0.0644 mas
Distance	73.9 ± 0.1 ly (22.66 ± 0.03 pc)
σ CrB B
Radial velocity (Rv)	−12.30 ± 0.06 km/s
Proper motion (μ)	RA: −291.118 mas/yr Dec.: −78.651 mas/yr
Parallax (π)	44.1475 ± 0.0237 mas
Distance	73.88 ± 0.04 ly (22.65 ± 0.01 pc)
σ CrB C
Radial velocity (Rv)	−16.30 ± 10 km/s
Proper motion (μ)	RA: −265.92 mas/yr Dec.: −83.63 mas/yr
Parallax (π)	42.8557 ± 0.3965 mas
Distance	76.1 ± 0.7 ly (23.3 ± 0.2 pc)
Orbit
Primary	σ CrB primary
Companion	σ CrB secondary
Period (P)	1.139791423(80)
Semi-major axis (a)	1.225 ± 0.013 mas
Eccentricity (e)	0.0
Inclination (i)	28.08 ± 0.34°
Longitude of the node (Ω)	207.93 ± 0.67°
Periastron epoch (T)	Tnode = 2450127.04855(20)
Argument of periastron (ω) (secondary)	0.0°
Orbit
Primary	σ CrB
Companion	σ CrB
Period (P)	726 ± 62 yr
Semi-major axis (a)	5.26 ± 0.35″
Eccentricity (e)	0.72 ± 0.01
Inclination (i)	32.3 ± 4.1°
Longitude of the node (Ω)	28.0 ± 0.5°
Periastron epoch (T)	B 1825.2 ± 1.5
Argument of periastron (ω) (primary)	237.3 ± 6.8°
Orbit
Primary	σ CrB Ca
Companion	σ CrB Cb
Period (P)	52 yr
Semi-major axis (a)	0.111″
Eccentricity (e)	0.36
Inclination (i)	59°
Longitude of the node (Ω)	30°
Periastron epoch (T)	B 1963.0
Argument of periastron (ω) (secondary)	127°
Details
σ CrB
Mass	1.0 M☉
Surface gravity (log g)	4.5 cgs
Temperature	5950 ± 100 K
Rotational velocity (v sin i)	3 ± 2 km/s
Age	1 to 3 Myr
σ CrB primary
Mass	1.137 ± 0.037 M☉
Radius	1.244 ± 0.050 R☉
Surface gravity (log g)	4.5 cgs
Temperature	6050 ± 150 K
Metallicity	0.0 dex
Rotational velocity (v sin i)	26 ± 1 km/s
Age	0.5 to 1.5 Gyr
σ CrB secondary
Mass	1.090 ± 0.036 M☉
Radius	1.244 ± 0.050 R☉
Surface gravity (log g)	4.5 cgs
Temperature	5870 ± 150 K
Metallicity	0.0 dex
Rotational velocity (v sin i)	26 ± 1 km/s
Age	0.5 to 1.5 Gyr
σ CrB C
Mass	0.423 ± 0.042 M☉
Radius	0.437 ± 0.020 R☉
Surface gravity (log g)	5.0 cgs
Temperature	3454 ± 63 K
Metallicity	−0.06 ± 0.03 dex
Age	2.95 Gyr
Other designations
σ CrB, 17 CrB, BD+34° 2750, HIP 79607 (only AB), SAO 65165, ADS 9979
σ CrB A: σ CrB, TZ CrB, GJ 9550B, HD 146361, HR 6064, CCDM J16147+3352A, WDS J16147+3352A, TYC 2583-1846-1
σ CrB B: σ CrB, GJ 9550A, HD 146362, HR 6063, CCDM J16147+3352B, WDS J16147+3352B, TYC 2583-1846-2
σ CrB C: GJ 9549, HIP 79551, WDS J16147+3352E, G 180-42
Database references
SIMBAD	σ CrB
	σ CrB
	σ CrB
	σ CrB C
ARICNS	σ CrB
	σ CrB
	σ CrB C

Sigma Coronae Borealis (σ CrB) is a star system in the constellation of Corona Borealis. It is a quintuple star system containing three sunlike main-sequence stars and two other low-mass stars. The combined visual magnitude is 5.3 and the system lies 74 light years from Earth. σ CrB A is the variable star TZ Coronae Borealis.

System components

The brightest components of Sigma Coronae Borealis form a visual binary with an angular separation of 7 arcsecond first resolved in the 19th century, and are designated σ Corona Borealis A and B. More recently, the designations σ and σ Corona Borealis have come into use. Somewhat confusingly, the brighter component A is referred to as σ because it has the higher right ascension. A third component, while being separated by 635″ (translating to a minimum distance of 14,000 au), has a similar parallax and proper motion to the brighter stars and is physically associated. It is known in the Washington Double Star Catalog (WDS), a compilation of observations of double stars, as component E, but it is usually called Sigma Coronae Borealis C.

Sigma Corona Borealis is a G-type main-sequence star like the Sun, and has similar parameters: a mass roughly equal to that of the Sun, and an effective temperature of 5950 K. A visual orbit has been calculated, with a period of about 730 years and a high eccentricity of 0.72.

Sigma Corona Borealis itself is a close binary. Here, the two stars are extremely close and orbit fairly quickly, every 1.14 days. This tiny separation of only 0.0279 au has allowed the two stars to exert tidal forces on each other, leading to synchronization of their rotation. They have also been classified as RS Canum Venaticorum variables (RS CVn)—young, active stars that show variability in their apparent magnitude due to starspots on their surfaces.

Despite Sigma Corona Borealis's two stars being separated only by about the diameter of each star, they were resolved using the CHARA optical interferometer at the Mount Wilson Observatory. As of 2006, it is the shortest-period binary ever to be resolved. The primary is 13.7% more massive than the Sun, while the secondary is 9.0% more massive than the Sun, and both are 24.4% wider than the Sun.

σ Coronae Borealis C, also known as HIP 79551, appears as a red dwarf with a spectral type of M2.5V. It too is a binary star, with a companion in a 52-year orbit. The companion has a mass of 0.10 M_☉ and has been detected through astrometry.

Optical companions

The Washington Double Star Catalog (WDS), a compilation of observations of double stars, lists several components to the main system. Two of those are listed in the WDS as components C, and D. As of 1984, component C was separated from the primary by 18″ along a position angle of 103° and as of 1996, component D was separated from the primary by 88″ along a position angle of 82°. However, both of them have different proper motions through space and are not related, just optical alignments.

Variability

The spectroscopic binary σ CrB is an RS Canum Venaticorum variable. It varies in brightness by 0.05 magnitudes every 1.139789 days, the same as the orbital period. The brightness changes are caused by variations in surface brightness on the stars, effectively giant sunspots. Variable star designations are not given to stars with Bayer designations, but in this case only one component of σ Coronae Borealis is identified as variable, so it has the designation TZ Coronae Borealis.

See also

• Xi Ursae Majoris, another quintuple containing an RS CVn binary

References

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2. ^ Høg, E.; et al. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27–L30. Bibcode:2000A&A...355L..27H.
3. ^ van Leeuwen, F.; et al. (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.
4. Zacharias, N.; et al. (2012). "The fourth US Naval Observatory CCD Astrograph Catalog (UCAC4)". VizieR On-line Data Catalog. 1322. Bibcode:2012yCat.1322....0Z.
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6. Gray, R. O.; Corbally, C. J.; Garrison, R. F.; McFadden, M. T.; Robinson, P. E. (2003). "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 Parsecs: The Northern Sample. I". The Astronomical Journal. 126 (4): 2048. arXiv:astro-ph/0308182. Bibcode:2003AJ....126.2048G. doi:10.1086/378365. S2CID 119417105.
7. ^ Rakos, K. D.; Albrecht, R.; Jenkner, H.; Kreidl, T.; Michalke, R.; Oberlerchner, D.; Santos, E.; Schermann, A.; Schnell, A.; Weiss, W. (1982). "Photometric and astrometric observations of close visual binaries". Astronomy and Astrophysics Supplement Series. 47 (221–235): 221. Bibcode:1982A&AS...47..221R.
8. ^ "* sig CrB". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 20 April 2017.
9. ^ Reid, I. Neill; Hawley, Suzanne L.; Gizis, John E. (1995). "The Palomar/MSU Nearby-Star Spectroscopic Survey. I. The Northern M Dwarfs -Bandstrengths and Kinematics". The Astronomical Journal. 110: 1838. Bibcode:1995AJ....110.1838R. doi:10.1086/117655.
10. ^ 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.{{cite journal}}: CS1 maint: unflagged free DOI (link)
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12. ^ Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
13. Hawley, Suzanne L.; Gizis, John E.; Reid, I. Neill (1996). "The Palomar/MSU Nearby Star Spectroscopic Survey.II.The Southern M Dwarfs and Investigation of Magnetic Activity". The Astronomical Journal. 112: 2799. Bibcode:1996AJ....112.2799H. doi:10.1086/118222.
14. Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
15. ^ Raghavan, Deepak; McAlister, Harold A.; Torres, Guillermo; Latham, David W.; Mason, Brian D.; Boyajian, Tabetha S.; Baines, Ellyn K.; Williams, Stephen J.; Brummelaar, Theo A. ten; Farrington, Chris D.; Ridgway, Stephen T.; Sturmann, Laszlo; Sturmann, Judit; Turner, Nils H. (2009). "The Visual Orbit of the 1.1-day Spectroscopic Binary σ Coronae Borealis from Interferometry at the CHARA Array". The Astrophysical Journal. 690 (1): 394–406. arXiv:0808.4015. Bibcode:2009ApJ...690..394R. doi:10.1088/0004-637X/690/1/394. S2CID 14638405.
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17. ^ Mann, Andrew W.; Feiden, Gregory A.; Gaidos, Eric; Boyajian, Tabetha; von Braun, Kaspar (2015). "How to Constrain Your M Dwarf: Measuring Effective Temperature, Bolometric Luminosity, Mass, and Radius". The Astrophysical Journal. 804 (1): 38. arXiv:1501.01635. Bibcode:2015ApJ...804...64M. doi:10.1088/0004-637X/804/1/64. S2CID 19269312.
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19. "* sig02 CrB". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 20 April 2017.
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21. "* sig CrB C". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 20 April 2017.
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External links

• Kaler, James B. "Sigma Coronae Borealis". Stars. University of Illinois.

• Corona Borealis
• Henry Draper Catalogue objects
• Bayer objects
• Objects with variable star designations
• Flamsteed objects
• Bright Star Catalogue objects
• F-type main-sequence stars
• G-type main-sequence stars
• Hipparcos objects
• Multiple star systems
• RS Canum Venaticorum variables
• Durchmusterung objects
• Gliese and GJ objects
• M-type main-sequence stars