{{Short description|Triple star system in the constellation Taurus}} {{Starbox begin}} {{Starbox image | image= {{Location mark | image=Taurus IAU.svg | alt=Chart showing the position of the stars in the constellation Taurus | float=center | width=300 | label= | position=right | mark=Red circle.svg | mark_width=10 | mark_link=HR 1099 | x%=81.8 | y%=74.2 }} | caption = Location of HR 1099 (circled) }} {{Starbox observe 2s | epoch = J2000 | constell = Taurus<ref name=constellation/> | component1 = A | ra1 = {{RA|03|36|47.291}}<ref name=GaiaDR3/> | dec1 = {{DEC|+00|35|15.94}}<ref name=GaiaDR3/> | appmag_v1 = 5.91<ref name=freund2018/> | component2 = B | ra2 = {{RA|03|36|46.844}}<ref name=GaiaDR3B/> | dec2 = {{DEC|+00|35|15.93}}<ref name=GaiaDR3B/> | appmag_v2 = 8.79<ref name=freund2018/> }} {{Starbox character | type = | class = K2:Vnk<ref name=Gray_et_al_2006/> {{nowrap|(K1 IV + G5 V + K3 V)}}<ref name=Lanza_et_al_2006/> | b-v = | u-b = | variable = RS CVn<ref name=Samus_et_al_2017/> }} {{Starbox astrometry | component1 = A | radial_v = −21.24{{±|6.62}}<ref name=GaiaDR3/> | prop_mo_ra = −32.894 | prop_mo_dec = −161.772 | pm_footnote = <ref name=GaiaDR3/> | parallax = 33.7528 | p_error = 0.0866 | parallax_footnote = <ref name=GaiaDR3/> | absmag_v = 3.6<ref name=freund2018/> | component2 = B | radial_v2 = {{val|-15.34|0.18}}<ref name=GaiaDR3B/> | prop_mo_ra2 = −34.359 | prop_mo_dec2 = −138.137 | pm_footnote2 = <ref name=GaiaDR3B/> | parallax2 = 33.8664 | p_error2 = 0.0226 | parallax_footnote2 = <ref name=GaiaDR3B/> | absmag_v2 = 6.5<ref name=freund2018/> }} {{Starbox orbit | reference = <ref name=Strassmeier_Bartus_2000/> | period_unitless = 2.83774 d | axis_unitless = {{val|10.3|ul=Solar radius}}<ref name=Donati_1999/> | eccentricity = 0.00 (assumed) | inclination = 38<ref name=Donati_et_al_2003/> | periastron = {{val|2442767.4|ul=HJD|fmt=commas}} | periarg = 0.00 (assumed) | k1 = 52.6 | k2 = 64.1 }} {{Starbox detail | source = | component1 = Component Aa | mass = 1.0<ref name=Donati_1999/> | radius = 3.7<ref name=Donati_1999/> | temperature = 4,750<ref name=Lanza_et_al_2006/> | luminosity = | gravity = 3.30<ref name=Lanza_et_al_2006/> | metal_fe = −0.16<ref name=pastel/> | rotational_velocity = 39<ref name=Donati_et_al_2003/> | rotation = | age_myr = | component2 = Component Ab | mass2 = 0.8<ref name=Donati_1999/> | radius2 = 1.1<ref name=Donati_1999/> | temperature2= 5,500<ref name=Lanza_et_al_2006/> | gravity2 = 4.26<ref name=Lanza_et_al_2006/> }} {{Starbox detail|no_heading=y | component1 = Component B | mass = 0.78<ref name=ticv8/> | radius = 0.78<ref name=ticv8/> | temperature = 4,829<ref name=ticv8/> | luminosity = 0.30<ref name=ticv8/> | gravity = 4.55<ref name=ticv8/> | metal_fe = +0.10<ref name=pastel/> | rotational_velocity = 4.1<ref name=Earle2017/> | rotation = | age_gyr = 2.2<ref name=GaiaDR3B/> }} {{Starbox catalog | names = {{odlist | name=STF 422 | V=V711 Tau | ADS=2644 | BD=+00°616 | GC=4311 | HD=22468 | HIP=16846 | HR=1099 | PPM=146726 | SAO=111291 | WDS=J03368+0035 }}<ref name=SIMBAD_A/><ref name=SIMBAD_B/> }} {{Starbox reference | Simbad=HD+22468 }} {{Starbox end}}
'''HR 1099''' is a triple star system in the equatorial constellation of Taurus, positioned {{val|11|ul=arcminute}} to the north of the star 10 Tauri.<ref name=Sinnott1997/> 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,<ref name=Samus_et_al_2017/> 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,<ref name=GaiaDR3/> 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 {{val|5.4|ul=arcsecond}}. (The separation was measured at {{val|6.7|u=arcsecond}} in 2016.)<ref name=Mason_et_al_2001/> 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.<ref name=Wilson_1963/> 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.<ref name=Wilson_1964/>
[[File:V711TauLightCurve.png|thumb|left|A light curve for V711 Tauri, plotted from ''TESS'' data<ref name=MAST/>]] 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.<ref name=Vogy_Penrod_1983/> 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.<ref name=Bopp_Fekel_1976/> Radio emission from the binary was detected by F. N. Owen in 1976.<ref name=Owen_1976/> It was shown to be a soft X-ray source in 1978 using the HEAO 1 satellite.<ref name=Walter_et_al_1978/>
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.<ref name=Lanza_et_al_2006/> The chromosphere of the subgiant is one of the most active known, with a deep convective zone powering the magnetic dynamo.<ref name=Petit_et_al_2004/><ref name=Gray_et_al_2006/> The G-type companion has a shallow convection zone and is less active.<ref name=Lanza_et_al_2006/>
In 1980, significant variations were found in some spectral features related to surface temperature, suggesting the presence of starspots.<ref name=Ramsey_Nations_1980/> Doppler imaging confirmed these starspots are associated with the K subgiant. (It was the first cool star to have its surface Doppler imaged.<ref name=Berdyugina_Henry_2007/>) The evidence suggests that the spots first appear at low latitude then migrated toward the poles.<ref name=Vogy_Penrod_1983/> These spots are much larger than they are on the Sun.<ref name=Lanza_et_al_2006/> About 70% of all spots have been observed at latitudes higher than 50°, particularly around the polar region.<ref name=Donati_et_al_2003/><ref name=Petit_et_al_2004/> A polar spot has persisted for at least twenty years.<ref name=Lanza_et_al_2006/>
The baseline apparent magnitudes of the two stars, after subtracting the effects of starspots, is 5.80 and 7.20.<ref name=Lanza_et_al_2006/> Long term monitoring indicates the subgiant has two activity cycles, similar to the 11-year solar cycle. A {{val|5.3|0.1|u=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.<ref name=Berdyugina_Henry_2007/>
==See also== * UX Arietis<ref name=Bopp_Fekel_1976/> {{Clear left}}
==References== {{reflist|30em|refs=
<ref name=SIMBAD_A>{{cite simbad | title=HD 22468A | access-date=2023-01-04 }}</ref> <ref name=SIMBAD_B>{{cite simbad | title=HD 22468B | access-date=2023-01-04 }}</ref>
<ref name=constellation>{{cite constellation|HR 1099}}</ref>
<ref name=GaiaDR3>{{Cite Gaia DR3|2031776202613700480}}</ref>
<ref name=GaiaDR3B>{{Cite Gaia DR3|3263936658312134272}}</ref>
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<ref name=Petit_et_al_2004>{{citation | postscript=. | title=Magnetic topology and surface differential rotation on the K1 subgiant of the RS CVn system HR 1099 | last1=Petit | first1=P. | last2=Donati | first2=J. -F. | last3=Wade | first3=G. A. | last4=Landstreet | first4=J. D. | last5=Bagnulo | first5=S. | last6=Lüftinger | first6=T. | last7=Sigut | first7=T. A. A. | last8=Shorlin | first8=S. L. S. | last9=Strasser | first9=S. | last10=Aurière | first10=M. | last11=Oliveira | first11=J. M. | display-authors=1 | journal=Monthly Notices of the Royal Astronomical Society | volume=348 | issue=4 | pages=1175–1190 | date=March 2004 | doi=10.1111/j.1365-2966.2004.07420.x | doi-access=free | arxiv=astro-ph/0312238 | bibcode=2004MNRAS.348.1175P | s2cid=119463091 }}</ref>
<ref name=Berdyugina_Henry_2007>{{citation | postscript=. | title=Butterfly Diagram and Activity Cycles in HR 1099 | last1=Berdyugina | first1=Svetlana V. | last2=Henry | first2=Gregory W. | journal=Astrophysical Journal | volume=659 | issue=2 | pages=L157–L160 | date=April 2007 | doi=10.1086/517881 | arxiv=astro-ph/0703530 | bibcode=2007ApJ...659L.157B | s2cid=14242208 }}</ref>
}}
==Further reading== {{Div col|small=yes|colwidth=20em}} *{{citation | postscript=. | title=Long-term variations in the X-ray activity of HR 1099 | display-authors=1 | last1=Perdelwitz | first1=V. | last2=Navarrete | first2=F. H. | last3=Zamponi | first3=J. | last4=Mennickent | first4=R. E. | last5=Völschow | first5=M. | last6=Robrade | first6=J. | last7=Schneider | first7=P. C. | last8=Schleicher | first8=D. R. G. | last9=Schmitt | first9=J. H. M. M. | journal=Astronomy & Astrophysics | volume=616 | id=A161 | date=August 2018 | pages=A161 | doi=10.1051/0004-6361/201732222 | arxiv=1806.03033 | bibcode=2018A&A...616A.161P | s2cid=55130058 }} *{{citation | postscript=. | title=A Multiwavelength Perspective of Flares on HR 1099: 4 Years of Coordinated Campaigns | last1=Osten | first1=Rachel A. | last2=Brown | first2=Alexander | last3=Ayres | first3=Thomas R. | last4=Drake | first4=Stephen A. | last5=Franciosini | first5=Elena | last6=Pallavicini | first6=Roberto | last7=Tagliaferri | first7=Gianpiero | last8=Stewart | first8=Ron T. | last9=Skinner | first9=Stephen L. | last10=Linsky | first10=Jeffrey L. | journal=Astrophysical Journal Supplement Series | display-authors=1 | volume=153 | issue=1 | pages=317–362 | date=July 2004 | doi=10.1086/420770 | arxiv=astro-ph/0402613 | bibcode=2004ApJS..153..317O | s2cid=119522693 }} *{{citation | postscript=. | title=Possible Corotation of the Milliarcsecond Radio Structure of the Close Binary HR 1099 | display-authors=1 | last1=Ransom | first1=R. R. | last2=Bartel | first2=N. | last3=Bietenholz | first3=M. F. | last4=Lebach | first4=D. E. | last5=Ratner | first5=M. I. | last6=Shapiro | first6=I. I. | last7=Lestrade | first7=J. -F. | journal=Astrophysical Journal | volume=572 | issue=1 | pages=487–502 | date=June 2002 | doi=10.1086/340300 | bibcode=2002ApJ...572..487R | s2cid=120225374 | doi-access=free }} *{{citation | postscript=. | title=Chandra, EUVE, HST, and VLA Multiwavelength Campaign on HR 1099: Instrumental Capabilities, Data Reduction, and Initial Results | last1=Ayres | first1=Thomas R. | last2=Brown | first2=Alexander | last3=Osten | first3=Rachel A. | last4=Huenemoerder | first4=David P. | last5=Drake | first5=Jeremy J. | last6=Brickhouse | first6=Nancy S. | last7=Linsky | first7= Jeffrey L. | display-authors=1 | journal=Astrophysical Journal | volume=549 | issue=1 | pages=554–577 | date=March 2001 | doi=10.1086/319051 | bibcode=2001ApJ...549..554A | s2cid=15938906 | doi-access=free }} *{{citation | postscript=. | title=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 | last1=Brinkman | first1=A. C. | last2=Behar | first2=E. | last3=Güdel | first3=M. | last4=Audard | first4=M. | last5=den Boggende | first5=A. J. F. | last6=Branduardi-Raymont | first6=G. | last7=Cottam | first7=J. | last8=Erd | first8=C. | last9=den Herder | first9=J. W. | last10=Jansen | first10=F. | last11=Kaastra | first11=J. S. | last12=Kahn | first12=S. M. | last13=Mewe | first13=R. | last14=Paerels | first14=F. B. S. | last15=Peterson | first15=J. R. | last16=Rasmussen | first16=A. P. | last17=Sakelliou | first17=I. | last18=de Vries | first18=C. | display-authors=1 | journal=Astronomy and Astrophysics | volume=365 | pages=L324–L328 | date=January 2001 | doi=10.1051/0004-6361:20000047 | arxiv=astro-ph/0011018 | bibcode=2001A&A...365L.324B | s2cid=15848464 }} *{{citation | postscript=. | title=The XMM-Newton view of stellar coronae: Flare heating in the coronae of HR 1099 | display-authors=1 | last1=Audard | first1=M. | last2=Güdel | first2=M. | last3=Mewe | first3=R. | journal=Astronomy and Astrophysics | volume=365 | pages=L318–L323 | date=January 2001 | doi=10.1051/0004-6361:20000085 | bibcode=2001A&A...365L.318A | doi-access=free }} *{{citation | postscript=. | display-authors=1 | title=Doppler Imagery of the Spotted RS CVn Star HR 1099 (= V711 Tau) from 1981 - 1992 | last1=Vogt | first1=Steven S. | last2=Hatzes | first2=Artie P. | last3=Misch | first3=Anthony A. | last4=Kurster | first4=M. | journal=Astrophysical Journal Supplement Series | date=April 1997 | volume=121 | page=547 | doi=10.1086/313195 | arxiv=astro-ph/9704191 | bibcode=1997astro.ph..4191V | s2cid=119515171 }} *{{citation | postscript=. | title=VLBI observations of a strong radio flare in HR 1099 | display-authors=1 | last1=Trigilio | first1=C. | last2=Umana | first2=G. | last3=Migenes | first3=V. | journal=Monthly Notices of the Royal Astronomical Society | volume=260 | pages=903–907 | date=February 1993 | issue=4 | doi=10.1093/mnras/260.4.903 | bibcode=1993MNRAS.260..903T | doi-access=free }} *{{citation | postscript=. | title=Photospheric imaging of the RS CVn system HR 1099. | last1=Donati | first1=J. -F. | last2=Brown | first2=S. 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{{Stars of Taurus}}
<!-- Properties -->
Category:G-type main-sequence stars Category:K-type main-sequence stars Category:K-type subgiants Category:RS Canum Venaticorum variables Category:Triple star systems <!-- Location & catalogues --> Category:Taurus (constellation) 1099 BD+00 0616 022468 016852 Tauri, V711