Astronomy:HR 1099
Observation data {{#ifeq:J2000|J2000.0 (ICRS)|Epoch J2000.0 Equinox J2000.0 (ICRS)| [[History:Epoch|Epoch J2000]] [[Astronomy:Equinox (celestial coordinates)|Equinox J2000}} | |
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Constellation | Taurus |
A | |
Right ascension | 03h 36m 47.291s[1] |
Declination | 00° 35′ 15.94″[1] |
Apparent magnitude (V) | 5.91[2] |
B | |
Right ascension | 03h 36m 46.844s[3] |
Declination | 00° 35′ 15.93″[3] |
Apparent magnitude (V) | 8.79[2] |
Characteristics | |
Spectral type | K2:Vnk[4] (K1 IV + G5 V + K3 V)[5] |
Variable type | RS CVn[6] |
Astrometry | |
A | |
Radial velocity (Rv) | −21.24±6.62[1] km/s |
Proper motion (μ) | RA: −32.894[1] mas/yr Dec.: −161.772[1] mas/yr |
Parallax (π) | 33.7528 ± 0.0866[1] mas |
Distance | 96.6 ± 0.2 ly (29.63 ± 0.08 pc) |
Absolute magnitude (MV) | 3.6[2] |
B | |
Radial velocity (Rv) | −15.34±0.18[3] km/s |
Proper motion (μ) | RA: −34.359 mas/yr Dec.: −138.137 mas/yr |
Parallax (π) | 33.8664 ± 0.0226[3] mas |
Distance | 96.31 ± 0.06 ly (29.53 ± 0.02 pc) |
Absolute magnitude (MV) | 6.5[2] |
Orbit[7] | |
Period (P) | 2.83774 d |
Semi-major axis (a) | 10.3 R☉[8] |
Eccentricity (e) | 0.00 (assumed) |
Inclination (i) | 38[9]° |
Periastron epoch (T) | 2,442,767.4 HJD |
Argument of periastron (ω) (secondary) | 0.00 (assumed)° |
Semi-amplitude (K1) (primary) | 52.6 km/s |
Semi-amplitude (K2) (secondary) | 64.1 km/s |
Details | |
Component Aa | |
Mass | 1.0[8] M☉ |
Radius | 3.7[8] R☉ |
Surface gravity (log g) | 3.30[5] cgs |
Temperature | 4,750[5] K |
Metallicity [Fe/H] | −0.16[10] dex |
Rotational velocity (v sin i) | 39[9] km/s |
Component Ab | |
Mass | 0.8[8] M☉ |
Radius | 1.1[8] R☉ |
Surface gravity (log g) | 4.26[5] cgs |
Temperature | 5,500[5] K |
Component B | |
Mass | 0.78[11] M☉ |
Radius | 0.78[11] R☉ |
Luminosity | 0.30[11] L☉ |
Surface gravity (log g) | 4.55[11] cgs |
Temperature | 4,829[11] K |
Metallicity [Fe/H] | +0.10[10] dex |
Rotational velocity (v sin i) | 4.1[12] km/s |
Age | 2.2[3] Gyr |
Other designations | |
Database references | |
SIMBAD | data |
HR 1099 is a triple star system in the equatorial constellation of Taurus, positioned 11′ to the north of the star 10 Tauri.[15] This system has the variable star designation V711 Tauri, while HR 1099 is the star's identifier from the Bright Star Catalogue. It ranges in brightness from a combined apparent visual magnitude of 5.71 down to 5.94,[6] which is bright enough to be dimly visible to the naked eye. The distance to this system is 96.6 light years based on parallax measurements,[1] but it is drifting closer with a radial velocity of about −15 km/s.
This system was discovered to be a double star by F. G. W. Struve in 1822, with the components A and B having an angular separation of 5.4″. (The separation was measured at 6.7″ in 2016.)[16] R. E. Wilson in 1953 determined that the brighter member of this pair, component A, has a variable radial velocity. In 1963, O. C. Wilson noted that the same component shows very high emission cores in the calcium H and K absorption lines.[17] Follow-up observations by O. C. Wilson in 1964 showed that the hydrogen–α line of component A is fully in emission and it displays moderate broadening due to rotation. He found a stellar classification of K3 V for component B, matching an ordinary K-type main-sequence star.[18]
Observations during 1974–1975 demonstrated that component A is a spectroscopic binary star system of the RS Canum Venaticorum variable class. Given its average magnitude of around 5.9, it is one of the brighter known variables of this type.[20] No eclipses were observed, but an orbital period of 2.838 days was determined. Most of the emission was found to be coming from the more massive member of this pair.[21] Radio emission from the binary was detected by F. N. Owen in 1976.[22] It was shown to be a soft X-ray source in 1978 using the HEAO 1 satellite.[23]
This double-lined spectroscopic binary system consists of an evolving K-type subgiant and an ordinary G-type main sequence star. The two stars are orbiting so close to each other that their tidal effects are giving them an elliptical shape. The subgiant is filling about 80% of its Roche lobe.[5] The chromosphere of the subgiant is one of the most active known, with a deep convective zone powering the magnetic dynamo.[24][4] The G-type companion has a shallow convection zone and is less active.[5]
In 1980, significant variations were found in some spectral features related to surface temperature, suggesting the presence of starspots.[25] Doppler imaging confirmed these starspots are associated with the K subgiant. (It was the first cool star to have its surface Doppler imaged.[26]) The evidence suggests that the spots first appear at low latitude then migrated toward the poles.[20] These spots are much larger than they are on the Sun.[5] About 70% of all spots have been observed at latitudes higher than 50°, particularly around the polar region.[9][24] A polar spot has persisted for at least twenty years.[5]
The baseline apparent magnitudes of the two stars, after subtracting the effects of starspots, is 5.80 and 7.20.[5] Long term monitoring indicates the subgiant has two activity cycles, similar to the 11-year solar cycle. A 5.3±0.1 year cycle is associated with symmetrical flip-flopping of the spotted area between hemispheres. The longer 15–16 year cycle is a periodic variation in the total spot area. The global magnetic field of the star may be precessing with respect to the axis of rotation.[26]
See also
References
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940 Gaia DR3 record for this source at VizieR.
- ↑ 2.0 2.1 2.2 2.3 Freund, S.; Robrade, J.; Schneider, P. C.; Schmitt, J. H. M. M. (2018), "The stellar content of the XMM-Newton slew survey", Astronomy and Astrophysics 614: A125, doi:10.1051/0004-6361/201732009, Bibcode: 2018A&A...614A.125F.
- ↑ 3.0 3.1 3.2 3.3 3.4 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940 Gaia DR3 record for this source at VizieR.
- ↑ 4.0 4.1 Gray, R. O. et al. (July 2006), "Contributions to the Nearby Stars (NStars) Project: spectroscopy of stars earlier than M0 within 40 pc—The Southern Sample", The Astronomical Journal 132 (1): 161–170, doi:10.1086/504637, Bibcode: 2006AJ....132..161G.
- ↑ 5.0 5.1 5.2 5.3 5.4 5.5 5.6 5.7 5.8 5.9 Lanza, A. F. et al. (August 2006), "Long-term starspot evolution, activity cycle, and orbital period variation of V711 Tauri (HR 1099)", Astronomy and Astrophysics 455 (2): 595–606, doi:10.1051/0004-6361:20064847, Bibcode: 2006A&A...455..595L.
- ↑ 6.0 6.1 Samus, N. N. et al. (2017), "General Catalogue of Variable Stars", Astronomy Reports, 5.1 61 (1): 80–88, doi:10.1134/S1063772917010085, Bibcode: 2017ARep...61...80S.
- ↑ Strassmeier, K. G.; Bartus, J. (February 2000), "Doppler imaging of stellar surface structure. XII. Rapid spot changes on the RS CVn binary V711 Tauri = HR 1099", Astronomy and Astrophysics 354: 537–550, Bibcode: 2000A&A...354..537S.
- ↑ 8.0 8.1 8.2 8.3 8.4 Donati, J. -F. (January 1999), "Magnetic cycles of HR 1099 and LQ Hydrae", Monthly Notices of the Royal Astronomical Society 302 (3): 457–481, doi:10.1046/j.1365-8711.1999.02096.x, Bibcode: 1999MNRAS.302..457D.
- ↑ 9.0 9.1 9.2 Donati, J. -F. et al. (November 2003), "Dynamo processes and activity cycles of the active stars AB Doradus, LQ Hydrae and HR 1099", Monthly Notices of the Royal Astronomical Society 345 (4): 1145–1186, doi:10.1046/j.1365-2966.2003.07031.x, Bibcode: 2003MNRAS.345.1145D.
- ↑ 10.0 10.1 Soubiran, Caroline et al. (2016), "The PASTEL catalogue: 2016 version", Astronomy & Astrophysics 591: A118, doi:10.1051/0004-6361/201628497, Bibcode: 2016A&A...591A.118S.
- ↑ 11.0 11.1 11.2 11.3 11.4 Stassun K.G. (October 2019), "The revised TESS Input Catalog and Candidate Target List", The Astronomical Journal 158 (4): 138, doi:10.3847/1538-3881/ab3467, Bibcode: 2019AJ....158..138S.
- ↑ Luck, R. Earle (January 2017), "Abundances in the Local Region II: F, G, and K Dwarfs and Subgiants", The Astronomical Journal 153 (1): 19, doi:10.3847/1538-3881/153/1/21, 21, Bibcode: 2017AJ....153...21L.
- ↑ "HD 22468A". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+22468A.
- ↑ "HD 22468B". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+22468B.
- ↑ Sinnott, Roger W.; Perryman, Michael A. C. (1997), Millennium Star Atlas, 1, Sky Publishing Corporation and the European Space Agency, p. 260, ISBN 0-933346-84-0.
- ↑ Mason, Brian D. et al. (2001), "The Washington Double Star Catalog", The Astronomical Journal 122 (6): 3466, doi:10.1086/323920, Bibcode: 2001AJ....122.3466M.
- ↑ Wilson, O. C. (October 1963), "A Probable Correlation Between Chromospheric Activity and Age in Main-Sequence Stars", Astrophysical Journal 138: 832, doi:10.1086/147689, Bibcode: 1963ApJ...138..832W.
- ↑ Wilson, O. C. (August 1964), "Chromospheric Activity and Lithium", Publications of the Astronomical Society of the Pacific 76 (451): 238, doi:10.1086/128091, Bibcode: 1964PASP...76..238W.
- ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. https://mast.stsci.edu/portal/Mashup/Clients/Mast/Portal.html.
- ↑ 20.0 20.1 Vogt, S. S.; Penrod, G. D. (September 1983), "Doppler imaging of spotted stars : application to the RS Canum Venaticorum star HR 1099", Publications of the Astronomical Society of the Pacific 95: 565–576, doi:10.1086/131208, Bibcode: 1983PASP...95..565V.
- ↑ 21.0 21.1 Bopp, B. W.; Fekel, F., Jr. (September 1976), "HR 1099: a new bright RS CVn variable", Astronomical Journal 81: 771–774, doi:10.1086/111951, Bibcode: 1976AJ.....81..771B.
- ↑ Owen, F. N. (March 1976), Marsden, B. G., ed., "HR 1099", IAU Circular 2929: 2, Bibcode: 1976IAUC.2929....2O.
- ↑ Walter, F.; Charles, P.; Bowyer, S. (August 1978), "Discovery of quiescent X-ray emission from HR 1099, RS CVn", Nature 274 (5671): 569–570, doi:10.1038/274569b0, Bibcode: 1978Natur.274R.569W.
- ↑ 24.0 24.1 Petit, P. et al. (March 2004), "Magnetic topology and surface differential rotation on the K1 subgiant of the RS CVn system HR 1099", Monthly Notices of the Royal Astronomical Society 348 (4): 1175–1190, doi:10.1111/j.1365-2966.2004.07420.x, Bibcode: 2004MNRAS.348.1175P.
- ↑ Ramsey, L. W.; Nations, H. L. (August 1980), "HR 1099 and the starspot hypothesis for RS CVn binaries", Astrophysical Journal 239: L121–L124, doi:10.1086/183306, Bibcode: 1980ApJ...239L.121R.
- ↑ 26.0 26.1 Berdyugina, Svetlana V.; Henry, Gregory W. (April 2007), "Butterfly Diagram and Activity Cycles in HR 1099", Astrophysical Journal 659 (2): L157–L160, doi:10.1086/517881, Bibcode: 2007ApJ...659L.157B.
Further reading
- Osten, Rachel A. et al. (July 2004), "A Multiwavelength Perspective of Flares on HR 1099: 4 Years of Coordinated Campaigns", Astrophysical Journal Supplement Series 153 (1): 317–362, doi:10.1086/420770, Bibcode: 2004ApJS..153..317O.
- Ransom, R. R. et al. (June 2002), "Possible Corotation of the Milliarcsecond Radio Structure of the Close Binary HR 1099", Astrophysical Journal 572 (1): 487–502, doi:10.1086/340300, Bibcode: 2002ApJ...572..487R.
- Ayres, Thomas R. et al. (March 2001), "Chandra, EUVE, HST, and VLA Multiwavelength Campaign on HR 1099: Instrumental Capabilities, Data Reduction, and Initial Results", Astrophysical Journal 549 (1): 554–577, doi:10.1086/319051, Bibcode: 2001ApJ...549..554A.
- Brinkman, A. C. et al. (January 2001), "First light measurements with the XMM-Newton reflection grating spectrometers: Evidence for an inverse first ionisation potential effect and anomalous Ne abundance in the Coronae of HR 1099", Astronomy and Astrophysics 365: L324–L328, doi:10.1051/0004-6361:20000047, Bibcode: 2001A&A...365L.324B.
- Audard, M. et al. (January 2001), "The XMM-Newton view of stellar coronae: Flare heating in the coronae of HR 1099", Astronomy and Astrophysics 365: L318–L323, doi:10.1051/0004-6361:20000085, Bibcode: 2001A&A...365L.318A.
- Vogt, Steven S. et al. (April 1997), "Doppler Imagery of the Spotted RS CVn Star HR 1099 (= V711 Tau) from 1981 - 1992", Astrophysical Journal Supplement Series 121: 547, doi:10.1086/313195, Bibcode: 1997astro.ph..4191V.
- Trigilio, C. et al. (February 1993), "VLBI observations of a strong radio flare in HR 1099", Monthly Notices of the Royal Astronomical Society 260 (4): 903–907, doi:10.1093/mnras/260.4.903, Bibcode: 1993MNRAS.260..903T.
- Donati, J. -F. et al. (November 1992), "Photospheric imaging of the RS CVn system HR 1099.", Astronomy and Astrophysics 265: 682–700, Bibcode: 1992A&A...265..682D.
- Donati, J. -F. et al. (June 1990), "Detection of a magnetic region of HR 1099", Astronomy and Astrophysics 232: L1–L4, Bibcode: 1990A&A...232L...1D.
- Rodono, M. et al. (April 1987), "Rotational modulation and flares on RS CVn and BY DRA stars. III. IUEobserations of V711 Tau = (HR 1099), II Peg and AR Lac", Astronomy and Astrophysics 176: 267–284, Bibcode: 1987A&A...176..267R.
- Lestrade, J. F. et al. (July 1984), "Detection of a sub-milliarcsecond radio component in the RS CVn system HR 1099", Astrophysical Journal 282: L23–L26, doi:10.1086/184296, Bibcode: 1984ApJ...282L..23L.
- Fekel, F. C., Jr. (May 1983), "Spectroscopy of V711 Tauri (= HR 1099) : fundamental properties and evidence for starspots", Astrophysical Journal 268: 274–281, doi:10.1086/160952, Bibcode: 1983ApJ...268..274F.
- Dorren, J. D. et al. (April 1981), "Starspots on V711 Tauri (HR 1099)", Astronomical Journal 86: 572–582, doi:10.1086/112918, Bibcode: 1981AJ.....86..572D.
- Brown, R. L.; Crane, P. C. (December 1978), "On the rapidly variable circular polarization of HR 1099 at radio frequencies", Astronomical Journal 83: 1504–1509, doi:10.1086/112352, Bibcode: 1978AJ.....83.1504B.
- Feldman, P. A. et al. (December 1978), "Discovery of a strong radio flaring from HR 1099", Astronomical Journal 83: 1471–1484, doi:10.1086/112346, Bibcode: 1978AJ.....83.1471F.
- Bopp, B. W.; Talcott, J. C. (December 1978), "Survey of Halpha emission in V711 Tau (HR 1099) and related Ca II emission binaries", Astronomical Journal 83: 1517–1521, doi:10.1086/112355, Bibcode: 1978AJ.....83.1517B.
- Gibson, D. M. et al. (December 1978), "VLA observations of HR 1099 during the 1977 international campaign", Astronomical Journal 83: 1495–1498, doi:10.1086/112350, Bibcode: 1978AJ.....83.1495G.
- Weiler, E. J. et al. (August 1980), "Coordinated ultraviolet, optical, and radio observations of HR 1099 and UX Arietis", Astrophysical Journal 239: L121–L124, doi:10.1086/183306, Bibcode: 1980ApJ...239L.121R.
- Owen, F. N. et al. (November 1976), "The detection of radio emission from the RS CVn binary HR 1099", Astrophysical Journal 210: L27–L30, doi:10.1086/182295, Bibcode: 1976ApJ...210L..27O.
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