Editing Ursa Minor (section)

=== Stars ===
{{See also|List of stars in Ursa Minor}}
The German cartographer [[Johann Bayer]] used the Greek letters [[alpha]] to [[theta]] to label the most prominent stars in the constellation, while his countryman [[Johann Elert Bode]] subsequently added [[iota]] through [[phi]]. Only [[lambda]] and pi remain in use, likely because of their proximity to the north celestial pole.<ref name=wagman /> Within the constellation's borders, there are 39 stars brighter than or equal to [[apparent magnitude]] 6.5.<ref name=tirionconst />{{efn|1=Objects of magnitude 6.5 are among the faintest visible to the unaided eye in suburban-rural transition night skies.<ref>{{cite web|url=http://www.skyandtelescope.com/resources/darksky/3304011.html?page=1&c=y|title=The Bortle Dark-Sky Scale|last=Bortle|first=John E.|date=February 2001|work=[[Sky & Telescope]]|access-date=29 November 2014|archive-date=31 March 2014|archive-url=https://web.archive.org/web/20140331202746/http://www.skyandtelescope.com/resources/darksky/3304011.html?page=1&c=y|url-status=dead}}</ref>}} 

The traditional names of the main seven in [[Johann Bayer]]'s ordering are:
# [[Polaris]]
# [[Kochab]]
# [[Pherkad]]
# [[Yildun]]
# [[Epsilon Ursae Minoris]] has no traditional name.
# [[Zeta Ursae Minoris]] has no traditional name.
# [[Eta Ursae Minoris]] has no traditional name.

Marking the Little Bear's tail,<ref name=wagman /> [[Polaris]], or Alpha Ursae Minoris, is the brightest star in the constellation, varying between apparent magnitudes 1.97 and 2.00 over a period of 3.97&nbsp;days.<ref name=AAVSOpol /> Located around 432&nbsp;[[light-year]]s away from Earth,<ref>{{cite web |url = http://simbad.u-strasbg.fr/simbad/sim-id?Ident=Alf+UMi&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id |title = Alpha Ursae Minoris – Classical Cepheid (Delta Cep Type) |work = SIMBAD Astronomical Database|publisher=Centre de Données astronomiques de Strasbourg |access-date = 19 August 2014}}</ref> it is a yellow-white [[supergiant]] that varies between [[spectral type]]s F7Ib and F8Ib,<ref name=AAVSOpol>{{cite web|url=http://www.aavso.org/vsx/index.php?view=detail.top&oid=37413 |title=Alpha Ursae Minoris |author=Otero, Sebastian Alberto |date=4 December 2007 |work=The International Variable Star Index |publisher=American Association of Variable Star Observers|access-date=16 May 2014}}</ref> and has around 6&nbsp;times the Sun's mass, 2,500&nbsp;times its luminosity, and 45&nbsp;times its radius. Polaris is the brightest [[Cepheid variable|Cepheid]] [[variable star]] visible from Earth. It is a triple star system, the supergiant primary star having two [[F-type main-sequence star|yellow-white main-sequence star]] companions that are 17 and 2,400&nbsp;[[astronomical unit]]s (AU) distant and take 29.6 and 42,000&nbsp;years respectively to complete one orbit.<ref name=kaleralpha>{{cite web| first1=James B. | last1=Kaler | title=Polaris | work=Stars | publisher=University of Illinois | url=http://stars.astro.illinois.edu/sow/polaris.html | access-date=19 August 2014}}</ref>

Traditionally called Kochab, Beta Ursae Minoris, at apparent magnitude 2.08, is slightly less bright than Polaris.<ref name=simbadbeta /> Located around 131&nbsp;light-years away from Earth,<ref name="vanLeeuwen2007">{{cite journal | first=F. | last=van Leeuwen | title=Validation of the New Hipparcos Reduction | journal=[[Astronomy and Astrophysics]] | volume=474 | issue=2 | pages=653–64 | date=2007 | bibcode=2007A&A...474..653V | doi=10.1051/0004-6361:20078357 | arxiv=0708.1752| s2cid=18759600 }}</ref>{{efn|1=Or more specifically 130.9±0.6&nbsp;light-years by parallax measurement.<ref name="vanLeeuwen2007" />}} it is an [[orange giant]]—an evolved star that has used up the hydrogen in its core and moved off the [[main sequence]]—of spectral type K4III.<ref name=simbadbeta>{{cite web |url = http://simbad.u-strasbg.fr/simbad/sim-id?Ident=Bet+UMi&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id |title = Beta Ursae Minoris – Variable Star |work = SIMBAD Astronomical Database|publisher=Centre de Données astronomiques de Strasbourg |access-date = 18 May 2014}}</ref> Slightly variable over a period of 4.6&nbsp;days, Kochab has had its mass estimated at 1.3&nbsp;times that of the Sun via measurement of these oscillations.<ref name=aaa483_3_L43>{{cite journal  | last1 = Tarrant | first1 = N.J. | last2 = Chaplin| first2 = W.J.| last3 = Elsworth| first3 = Y.| last4 = Spreckley | first4 = S.A.| last5 = Stevens| first5 = I.R.| title = Oscillations in ß Ursae Minoris. Observations with SMEI | journal = Astronomy and Astrophysics | volume = 483 | issue = #3 | pages = L43–L46  |date=June 2008 | doi = 10.1051/0004-6361:200809738 | bibcode = 2008A&A...483L..43T | arxiv = 0804.3253 | s2cid = 53546805 }}</ref> Kochab is 450 times more luminous than the Sun and has 42 times its diameter, with a surface temperature of approximately 4,130&nbsp;K.<ref name=kalerbeta>{{cite web| first1=James B. | last1=Kaler | title=Kochab | work=Stars | publisher=University of Illinois | url=http://stars.astro.illinois.edu/sow/kochab.html | access-date=19 August 2014}}</ref> Estimated to be around 2.95&nbsp;billion years old, ±1&nbsp;billion years, Kochab was announced to have a planetary companion around 6.1&nbsp;times as massive as [[Jupiter]] with an orbit of 522&nbsp;days.<ref>{{cite journal |title=Planetary Companions in K giants β Cancri, μ Leonis, and β Ursae Minoris | author=Lee, B.-C. | author2=Han, I. | author3=Park, M.-G. | author4=Mkrtichian, D.E. | author5=Hatzes, A.P. | author6=Kim, K.-M.| journal = Astronomy and Astrophysics| volume = 566| id=A67 | pages=7 | date = 2014| doi =10.1051/0004-6361/201322608 | bibcode=2014A&A...566A..67L|arxiv = 1405.2127 | s2cid=118631934 }}</ref>

[[File:Ursa Major - Ursa Minor - Polaris.jpg|thumb|300px|Ursa Minor and Ursa Major in relation to Polaris]]
Traditionally known as Pherkad, Gamma Ursae Minoris has an apparent magnitude that varies between 3.04 and 3.09 roughly every 3.4&nbsp;hours.<ref name=AAVSOgam>{{cite web|url=http://www.aavso.org/vsx/index.php?view=detail.top&oid=37414 |title=Gamma Ursae Minoris |author=Watson, Christopher |date=4 January 2010 |work=The International Variable Star Index |publisher=American Association of Variable Star Observers|access-date=18 May 2014}}</ref> It and Kochab have been termed the "guardians of the pole star".<ref name=Arnold99 /> A white bright giant of spectral type A3II-III,<ref name=AAVSOgam /> with around 4.8&nbsp;times the Sun's mass, 1,050&nbsp;times its luminosity and 15&nbsp;times its radius,<ref name=kalergamma>{{cite web| first1=James B. | last1=Kaler | title=Pherkad | work=Stars | publisher=University of Illinois | url=http://stars.astro.illinois.edu/sow/pherkad.html | access-date=18 May 2014 |date=20 December 2013}}</ref> it is 487±8 light-years distant from Earth.<ref name="vanLeeuwen2007" /> Pherkad belongs to a class of stars known as [[Delta Scuti variable]]s<ref name=AAVSOgam />—short period (six hours at most) pulsating stars that have been used as [[Cosmic distance ladder#Standard candles|standard candles]] and as subjects to study [[asteroseismology]].<ref>{{cite web|url=http://www.aavso.org/vsots_delsct|title=Delta Scuti and the Delta Scuti Variables|last=Templeton|first=Matthew |date=16 July 2010|work=Variable Star of the Season|publisher=AAVSO (American Association of Variable Star Observers)|access-date=19 August 2014}}</ref> Also possibly a member of this class is [[Zeta Ursae Minoris]],<ref name=kalerzet /> a white star of spectral type A3V,<ref name=SIMBADzet>{{cite web |url = http://simbad.u-strasbg.fr/simbad/sim-id?Ident=Zet+UMi&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id |title = Zeta Ursae Minoris – Variable Star |work = SIMBAD Astronomical Database|publisher=Centre de Données astronomiques de Strasbourg |access-date = 21 June 2014}}</ref> which has begun cooling, expanding and brightening. It is likely to have been a B3 main-sequence star and is now slightly variable.<ref name=kalerzet>{{cite web| first1=James B. | last1=Kaler | title=Alifa al Farkadain | work=Stars | publisher=University of Illinois | url=http://stars.astro.illinois.edu/sow/alifa.html | access-date=21 June 2014}}</ref> At magnitude 4.95 the dimmest of the seven stars of the Little Dipper is [[Eta Ursae Minoris]].<ref name=kalereta /> A yellow-white main-sequence star of spectral type F5V, it is 97 light-years distant.<ref name=SIMBADeta>{{cite web |url = http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=Eta+Ursae+Minoris&submit=SIMBAD+search |title = Eta Ursae Minoris |work = SIMBAD Astronomical Database|publisher=Centre de Données astronomiques de Strasbourg |access-date = 30 July 2014}}</ref> It is double the Sun's diameter, 1.4&nbsp;times as massive, and shines with 7.4&nbsp;times its luminosity.<ref name=kalereta>{{cite web| first1=James B. | last1=Kaler | title=Anwar al Farkadain | work=Stars | publisher=University of Illinois | url=http://stars.astro.illinois.edu/sow/anwar.html | access-date=21 June 2014}}</ref> Nearby Zeta lies 5.00-magnitude [[Theta Ursae Minoris]]. Located 860 ± 80&nbsp;light-years distant,<ref name=SIMBADtet>{{cite web |url = http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=Theta+Ursae+Minoris&submit=SIMBAD+search |title = Theta Ursae Minoris – Variable Star |work = SIMBAD Astronomical Database|publisher=Centre de Données astronomiques de Strasbourg |access-date = 30 July 2014}}</ref> it is an orange giant of spectral type K5III that has expanded and cooled off the main sequence, and has an estimated diameter around 4.8&nbsp;times that of the Sun.<ref name=aaa367_521>{{cite journal | last1=Pasinetti Fracassini | first1=L. E. | last2=Pastori | first2=L. | last3=Covino | first3=S. | last4=Pozzi | first4=A. | title=Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS) – Third edition – Comments and statistics | journal=Astronomy and Astrophysics | volume=367 | pages=521–24 |date=February 2001 | issue=2 | doi=10.1051/0004-6361:20000451 | bibcode=2001A&A...367..521P | arxiv=astro-ph/0012289| s2cid=425754 }}</ref>

Making up the handle of the Little Dipper are [[Delta Ursae Minoris]], or Yildun,<ref name="IAU-LSN">{{cite web | url=https://www.iau.org/public/themes/naming_stars/ | title=Naming Stars |publisher=IAU.org |access-date=8 August 2018}}</ref> and [[Epsilon Ursae Minoris]]. Just over 3.5 degrees from the north celestial pole, Delta is a [[A-type main-sequence star|white main-sequence star]] of spectral type [[stellar classification|A1V]] with an apparent magnitude of 4.35,<ref>{{cite web |url = http://simbad.u-strasbg.fr/simbad/sim-id?Ident=Delta+UMi&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id |title = Delta Ursae Minoris |work = SIMBAD Astronomical Database|publisher=Centre de Données astronomiques de Strasbourg |access-date = 21 June 2014}}</ref> located 172±1 light-years from Earth.<ref name="vanLeeuwen2007" /> It has around 2.8 times the diameter and 47 times the luminosity of the Sun.<ref name=kalerdel>{{cite web| first1=James B. | last1=Kaler | title=Yildun | work=Stars | publisher=University of Illinois | url=http://stars.astro.illinois.edu/sow/yildun.html | access-date=30 July 2014}}</ref> A triple star system,<ref name=kalereps>{{cite web| first1=James B. | last1=Kaler | title=Epsilon Ursae Minoris | work=Stars | publisher=University of Illinois | url=http://stars.astro.illinois.edu/sow/epsumi.html | access-date=21 June 2014}}</ref> Epsilon Ursae Minoris shines with a combined average light of magnitude 4.22.<ref name=SIMBADeps>{{cite web |url = http://simbad.u-strasbg.fr/simbad/sim-id?Ident=Eps+UMi&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id |title = Epsilon Ursae Minoris – Variable of RS CVn type |work = SIMBAD Astronomical Database|publisher=Centre de Données astronomiques de Strasbourg |access-date = 21 June 2014}}</ref> A yellow giant of spectral type G5III,<ref name=SIMBADeps /> the primary is a [[RS Canum Venaticorum variable]] star. It is a spectroscopic binary, with a companion 0.36&nbsp;AU distant, and a third star—an orange main-sequence star of spectral type K0—8100&nbsp;AU distant.<ref name=kalereps />

Located close to Polaris is [[Lambda Ursae Minoris]], a [[red giant]] of spectral type M1III. It is a [[semiregular variable]] varying between magnitudes 6.35 and 6.45.<ref name=AAVSOlam>{{cite web|url=http://www.aavso.org/vsx/index.php?view=detail.top&oid=37416 |title=Lambda Ursae Minoris |author=Watson, Christopher |date=4 January 2010 |work=The International Variable Star Index|publisher=American Association of Variable Star Observers|access-date=21 June 2014}}</ref> The northerly nature of the constellation means that the variable stars can be observed all year: The red giant [[R Ursae Minoris]] is a semiregular variable varying from magnitude 8.5 to 11.5 over 328&nbsp;days, while [[S Ursae Minoris]] is a long-period variable that ranges between magnitudes 8.0 and 11 over 331&nbsp;days.<ref name="Levy 1998">{{cite book|last=Levy|first=David H.|title=Observing Variable Stars: A Guide for the Beginner|publisher=Cambridge University Press|location=Cambridge, UK|date=1998|page=133|isbn=978-0-521-62755-9|url=https://books.google.com/books?id=5-O2cd937FMC&pg=PA133}}</ref> Located south of Kochab and Pherkad towards Draco is [[RR Ursae Minoris]],<ref name=Arnold99>{{cite book|author=Arnold, H. J. P.|author2= Doherty, Paul|author3= Moore, Patrick |title=The Photographic Atlas of the Stars|publisher=CRC Press|location=Boca Raton, Florida|date=1999|page=148|isbn=978-0-7503-0654-6|url=https://books.google.com/books?id=YjcvJUfnWBAC&pg=PA148}}</ref> a red giant of spectral type M5III that is also a semiregular variable ranging from magnitude 4.44 to 4.85 over a period of 43.3&nbsp;days.<ref name=AAVSOrr>{{cite web|url=http://www.aavso.org/vsx/index.php?view=detail.top&oid=37384 |title=RR Ursae Minoris |author=Otero, Sebastian Alberto |date=16 November 2009 |work=The International Variable Star Index |publisher=American Association of Variable Star Observers|access-date=18 May 2014}}</ref> [[T Ursae Minoris]] is another red-giant variable star that has undergone a dramatic change in status—from being a long-period (Mira) variable ranging from magnitude 7.8 to 15 over 310–315 days, to being a semiregular variable.<ref name="Uttenthaler">{{cite journal|author=Uttenthaler, S.|author2=van Stiphout, K.|author3=Voet, K.|author4=van Winckel, H.|author5=van Eck, S.|author6=Jorissen, A.|author7=Kerschbaum, F.|author8=Raskin, G.|author9=Prins, S.|author10=Pessemier, W.|author11=Waelkens, C.|author12=Frémat, Y.|author13=Hensberge, H.|author14=Dumortier, L.|author15=Lehmann, H.|date=2011|title=The Evolutionary State of Miras with Changing Pulsation Periods|journal=Astronomy and Astrophysics|volume=531|pages=A88|bibcode=2011A&A...531A..88U|arxiv = 1105.2198 |doi = 10.1051/0004-6361/201116463 |s2cid=56226953}}</ref> The star is thought to have undergone a [[Helium flash#shell helium flash|shell helium flash]]—a point where the shell of helium around the star's core reaches a critical mass and ignites—marked by its abrupt change in variability in 1979.<ref name="mattei95">{{cite journal|author=Mattei, Janet A.|author2=Foster, Grant|date=1995|title=Dramatic Period Decrease in T Ursae Minoris|journal=The Journal of the American Association of Variable Star Observers|volume=23|issue=2|pages=106–16|bibcode=1995JAVSO..23..106M}}</ref> [[Z Ursae Minoris]] is a faint variable star that suddenly dropped 6&nbsp;magnitudes in 1992 and was identified as one of a rare class of stars—[[R Coronae Borealis variable]]s.<ref>{{cite journal|author= Benson, Priscilla J.|author2= Clayton, Geoffrey C.|author3= Garnavich, Peter|author4= Szkody, Paula |title= Z Ursa Minoris – a New R Coronae Borealis Variable |journal= [[The Astronomical Journal]] | volume= 108|issue= #1| pages= 247–50 | date=1994 |bibcode=1994AJ....108..247B|doi = 10.1086/117063 |doi-access= free}}</ref>

Eclipsing variables are star systems that vary in brightness because of one star passing in front of the other rather than from any intrinsic change in luminosity. [[W Ursae Minoris]] is one such system, its magnitude ranging from 8.51 to 9.59 over 1.7 days.<ref name=AAVSOW>{{cite web|url=http://www.aavso.org/vsx/index.php?view=detail.top&oid=37380 |title=W Ursae Minoris |author=Watson, Christopher |date=4 January 2010  |work=The International Variable Star Index |publisher=American Association of Variable Star Observers|access-date=18 July 2015}}</ref> The combined spectrum of the system is A2V, but the masses of the two component stars are unknown. A slight change in the orbital period in 1973 suggests there is a third component of the multiple star system—most likely a [[red dwarf]]—with an orbital period of 62.2±3.9 years.<ref>{{cite journal | title=Period Analysis of Three Close Binary Systems: TW And, TT Her and W UMi |author1=Kreiner, J. M. |author2=Pribulla, T. |author3=Tremko, J. |author4=Stachowski, G. S. |author5=Zakrzewski, B. | journal =Monthly Notices of the Royal Astronomical Society | volume = 383 | issue = #4 |pages= 1506–12|date=2008 |doi=10.1111/j.1365-2966.2007.12652.x |bibcode=2008MNRAS.383.1506K|doi-access=free }}</ref> [[RU Ursae Minoris]] is another example, ranging from 10 to 10.66 over 0.52&nbsp;days.<ref name=AAVSOru>{{cite web|url=http://www.aavso.org/vsx/index.php?view=detail.top&oid=37387 |title=RU Ursae Minoris |author=Watson, Christopher |date=4 January 2010  |work=The International Variable Star Index |publisher=American Association of Variable Star Observers|access-date=18 July 2015}}</ref> It is a [[semidetached binary|semidetached]] system, as the secondary star is filling its [[Roche lobe]] and transferring matter to the primary.<ref name="Manimanis">{{cite journal|title=A Photometric Study of the Near-contact System RU Ursae Minoris |author1=Manimanis, V. N. |author2=Niarchos, P. G. | journal=Astronomy and Astrophysics |volume=369 |issue=3 |pages=960–64 |date=2001|doi=10.1051/0004-6361:20010178 |bibcode=2001A&A...369..960M|doi-access=free }}</ref>

[[RW Ursae Minoris]] is a [[cataclysmic variable]] star system that flared up as a [[nova]] in 1956, reaching magnitude 6. In 2003, it was still two magnitudes brighter than its baseline, and dimming at a rate of 0.02 magnitude a year. Its distance has been calculated as 5,000±800&nbsp;parsecs (16,300&nbsp;light-years), which puts its location in the [[galactic halo]].<ref name=bianchini2003>{{cite journal |title = RW Ursae Minoris (1956): An Evolving Postnova System |author =Bianchini, A. |author2 =Tappert, C. |author3 = Canterna, R. |author4 =Tamburini, F. |author5 =Osborne, H. |author6 =Cantrell, K. |journal= [[Publications of the Astronomical Society of the Pacific]] |volume =115 |issue= #809 | pages = 811–18 | bibcode=2003PASP..115..811B|doi = 10.1086/376434 |year =2003 |doi-access =free }}</ref>

Taken from the villain in ''[[The Magnificent Seven]]'', [[Calvera (X-ray source)|Calvera]] is the nickname given to an [[astrophysical X-ray source|X-ray source]] known as 1RXS J141256.0+792204 in the ''[[ROSAT]] All-Sky Survey Bright Source Catalog'' (RASS/BSC).<ref>{{cite news|url=http://news.bbc.co.uk/2/hi/science/nature/6955769.stm|title=Rare Dead Star Found Near Earth|publisher=BBC |work= BBC News: Science/Nature |date=20 August 2007|access-date=21 August 2007|archive-date=13 July 2014 |archive-url=https://web.archive.org/web/20140713133234/http://news.bbc.co.uk/2/hi/science/nature/6955769.stm|url-status=live}}</ref> It has been identified as an isolated [[neutron star]], one of the closest of its kind to Earth.<ref>{{cite journal| author=Rutledge, Robert| author2=Fox, Derek| author3=Shevchuk, Andrew |date=2008 |title=Discovery of an Isolated Compact Object at High Galactic Latitude | journal=[[The Astrophysical Journal]]| volume= 672| issue= #2 |pages= 1137–43 |bibcode=2008ApJ...672.1137R|arxiv = 0705.1011 |doi = 10.1086/522667 | s2cid=7915388}}</ref> Ursa Minor has two enigmatic [[white dwarf]]s. Documented on January 27, 2011, [[H1504+65]] is a faint (magnitude 15.9) star with the hottest surface temperature—200,000 K—yet discovered for a white dwarf. Its atmosphere, composed of roughly half carbon, half oxygen and 2% neon, is devoid of hydrogen and helium—its composition unexplainable by current models of stellar evolution.<ref>{{cite journal|last=Werner|first=K.|author2=Rauch, T.|date=2011|title=UV Spectroscopy of the Hot Bare Stellar Core H1504+65 with the HST Cosmic Origins Spectrograph|journal=[[Astrophysics and Space Science]]|volume=335|issue=1|pages=121–24|doi=10.1007/s10509-011-0617-x|bibcode = 2011Ap&SS.335..121W |s2cid=116910726}}</ref> [[WD 1337+705]] is a cooler white dwarf that has magnesium and silicon in its spectrum, suggesting a companion or circumstellar disk, though no evidence for either has come to light.<ref>{{cite journal|author1=Dickinson, N. J. |author2=Barstow, M. A. |author3=Welsh, B. Y. |author4=Burleigh, M. |author5=Farihi, J. |author6=Redfield, S. |author7=Unglaub, K. |date=2012|title=The Origin of Hot White Dwarf Circumstellar Features|journal=[[Monthly Notices of the Royal Astronomical Society]] |volume=423|issue=2|pages=1397–1410| doi=10.1111/j.1365-2966.2012.20964.x |doi-access=free |bibcode=2012MNRAS.423.1397D|arxiv = 1203.5226 |s2cid=119212643 }}</ref> [[WISE 1506+7027]] is a [[brown dwarf]] of spectral type T6 that is a mere {{val|11.1|+2.3|-1.3}} light-years away from Earth.<ref name="Marsh2013">{{cite journal | last=Marsh |first=Kenneth A. | author2=Wright, Edward L. | author3=Kirkpatrick, J. Davy | author4=Gelino, Christopher R. | author5=Cushing, Michael C. | author6=Griffith, Roger L. | author7=Skrutskie, Michael F. | author8=Eisenhardt, Peter R. | date=2013 | title=Parallaxes and Proper Motions of Ultracool Brown Dwarfs of Spectral Types Y and Late T | journal=[[The Astrophysical Journal]] | volume=762 | issue=2 | pages=119 | arxiv=1211.6977 | bibcode=2013ApJ...762..119M | doi=10.1088/0004-637X/762/2/119|s2cid=42923100 }}</ref> A faint object of magnitude 14, it was discovered by the [[Wide-field Infrared Survey Explorer]] (WISE) in 2011.<ref name="Kirkpatrick2011">{{cite journal |doi=10.1088/0067-0049/197/2/19 |author-link=J. Davy Kirkpatrick |last1=Kirkpatrick |first1=J. Davy |last2=Cushing |first2=Michael C. |last3=Gelino |first3=Christopher R. |last4=Griffith |first4=Roger L. |last5=Skrutskie |first5=Michael F. |last6=Marsh |first6=Kenneth A. |last7=Wright |first7=Edward L. |last8=Mainzer |first8=Amy K. |last9=Eisenhardt |first9=Peter R. |last10=McLean |first10=Ian S. |last11=Thompson |first11=Maggie A. |last12=Bauer |first12=James M. |last13=Benford |first13=Dominic J. |last14=Bridge |first14=Carrie R. |last15=Lake |first15=Sean E. |last16=Petty |first16=Sara M. |last17=Stanford |first17=Spencer Adam |last18=Tsai |first18=Chao-Wei |last19=Bailey |first19=Vanessa |last20=Beichman |first20=Charles A. |last21=Bloom |first21=Joshua S. |last22=Bochanski |first22=John J. |last23=Burgasser |first23=Adam J. |last24=Capak |first24=Peter L. |last25=Cruz |first25=Kelle L. |last26=Hinz |first26=Philip M. |last27=Kartaltepe |first27=Jeyhan S. |last28=Knox |first28=Russell P. |last29=Manohar |first29=Swarnima |last30=Masters |first30=Daniel |last31=Morales-Calderon |first31=Maria |last32=Prato |first32=Lisa A. |last33=Rodigas |first33=Timothy J. |last34=Salvato |first34=Mara |last35=Schurr |first35=Steven D. |last36=Scoville |first36=Nicholas Z. |last37=Simcoe |first37=Robert A. |last38=Stapelfeldt |first38=Karl R. |last39=Stern |first39=Daniel |last40=Stock |first40=Nathan D. |last41=Vacca |first41=William D. |title=The First Hundred Brown Dwarfs Discovered by the Wide-field Infrared Survey Explorer (WISE) |date=2011 |journal=[[The Astrophysical Journal Supplement]] |volume=197 |issue=2 |pages=19 |arxiv=1108.4677v1 |bibcode=2011ApJS..197...19K |s2cid=16850733 }}</ref>

Kochab aside, three more stellar systems have been discovered to contain planets. [[11 Ursae Minoris]] is an orange giant of spectral type K4III around 1.8&nbsp;times as massive as the Sun. Around 1.5&nbsp;billion years old, it has cooled and expanded since it was an A-type main-sequence star. Around 390 light-years distant, it shines with an apparent magnitude of 5.04. A planet around 11 times the mass of Jupiter was discovered in 2009 orbiting the star with a period of 516 days.<ref name="Döllinger2009">{{cite journal | title=Planetary Companions around the K Giant Stars 11 Ursae Minoris and HD 32518 | last1=Döllinger | first1=M. P. | last2=Hatzes | first2=A.P. | last3=Pasquini | first3=L. | last4=Guenther | first4=E. W. | last5=Hartmann | first5=M. | journal=Astronomy and Astrophysics | volume=505 | issue=3 | pages=1311–17 | date=2009 | arxiv=0908.1753 | bibcode=2009A&A...505.1311D | doi=10.1051/0004-6361/200911702 | s2cid=9686080 }}</ref> [[HD 120084]] is another evolved star, a yellow giant of spectral type G7III, around 2.4 times the mass of the Sun. It has a planet 4.5 times the mass of Jupiter, with one of the most eccentric planetary orbits (e = 0.66), discovered by precisely measuring the radial velocity of the star in 2013.<ref>{{cite journal | arxiv=1304.4328  |title=Planetary Companions to Three Evolved Intermediate-Mass Stars: HD 2952, HD 120084, and omega Serpentis| url=https://archive.org/details/arxiv-1304.4328  |author= Sato, Bun'ei|author2= Omiya, Masashi|author3=  Harakawa, Hiroki|author4=  Liu, Yu-Juan|author5=  Izumiura, Hideyuki|author6=  Kambe, Eiji|author7=  Takeda, Yoichi|author8=  Yoshida, Michitoshi|author9=  Itoh, Yoichi|author10=  Ando, Hiroyasu|author11=  Kokubo, Eiichiro|author12=  Ida, Shigeru | journal= [[Publications of the Astronomical Society of Japan]] |pages = [https://archive.org/details/arxiv-1304.4328/page/n0 1]–15 |date=2013|volume=65|issue=4|bibcode = 2013PASJ...65...85S |doi = 10.1093/pasj/65.4.85 |s2cid=119248666}}</ref> [[HD 150706]] is a sunlike star of spectral type G0V some 89 light-years distant from the Solar System. It was thought to have a planet as massive as Jupiter at a distance of 0.6 AU, but this was discounted in 2007.<ref>{{cite journal|author=Wright, J.T.|author2=Marcy, G.W.|author3=Fischer, D. A.|author4=Butler, R. P.|author5=Vogt, S. S.|author6=Tinney, C. G.|author7=Jones, H. R. A.|author8=Carter, B. D.|author9=Johnson, J. A.|author10=McCarthy, C.|author11=Apps, K.|date=2007|title=Four New Exoplanets and Hints of Additional Substellar Companions to Exoplanet Host Stars|journal=The Astrophysical Journal|volume=657|issue=1|pages=533–45|doi=10.1086/510553 |bibcode=2007ApJ...657..533W|arxiv = astro-ph/0611658 |s2cid=35682784}}</ref> A further study published in 2012 showed that it has a companion around 2.7 times as massive as Jupiter that takes around 16 years to complete an orbit and is 6.8 AU distant from its star.<ref name="Boisse2012">{{citation |doi=10.1051/0004-6361/201118419 |arxiv=1205.5835 |url=http://www.aanda.org/articles/aa/full_html/2012/09/aa18419-11/aa18419-11.html |title=The SOPHIE search for northern extrasolar planets V. Follow-up of ELODIE candidates: Jupiter-analogs around Sun-like stars |year=2012 |last1=Boisse |first1=Isabelle |last2=Pepe |first2=Francesco |last3=Perrier |first3=Christian |last4=Queloz |first4=Didier |last5=Bonfils |first5=Xavier |last6=Bouchy |first6=François |last7=Santos |first7=Nuno C. |last8=Arnold |first8=Luc |last9=Beuzit |first9=Jean-Luc |last10=Dìaz |first10=Rodrigo F. |last11=Delfosse |first11=Xavier |last12=Eggenberger |first12=Anne |last13=Ehrenreich |first13=David |last14=Forveille |first14=Thierry |last15=Hébrard |first15=Guillaume |last16=Lagrange |first16=Anne-Marie |last17=Lovis |first17=Christophe |last18=Mayor |first18=Michel |last19=Moutou |first19=Claire |last20=Naef |first20=Dominique |last21=Santerne |first21=Alexandre |last22=Ségransan |first22=Damien |last23=Sivan |first23=Jean-Pierre |last24=Udry |first24=Stéphane |journal=Astronomy and Astrophysics |volume=545 |pages=A55 |bibcode=2012A&A...545A..55B |s2cid=119109836 }}</ref>