36 Ursae Majoris: Difference between revisions

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m Hmmm, doesn't say Simbad any more
binary system, companion is known as 36 UMa B, add it to the starbox
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| name = 36 Ursae Majoris
| name = 36 Ursae Majoris
}}
}}
{{Starbox observe
{{Starbox observe 2s
| epoch = [[J2000.0]]
| epoch = [[J2000.0]]
| constell = [[Ursa Major]]
| constell = [[Ursa Major]]
| component1 = A
⚫
| ra = {{RA|10|30|37.5798}}<ref name=aaa474_2_653/>
| dec = {{DEC|+55|58|49.931}}<ref name=aaa474_2_653/>
| ra1 = {{RA|10|30|37.5793}}<ref name=dr3a/>
| appmag_v = 4.82<ref name=clpl4_99/>
| dec1 = {{DEC|+55|58|49.940}}<ref name=dr3a/>
⚫
| appmag_v1 = 4.82<ref name=clpl4_99/>
| component2 = B
⚫
| ra2 = {{RA|10|30|25.3089}}<ref name=dr3b/>
| dec2 = {{DEC|+55|59|56.855}}<ref name=dr3b/>
⚫
| appmag_v2 = 8.86<ref name=ticv8/>
}}
}}
{{Starbox character
{{Starbox character
| component1 = A
| type = [[main sequence]]
| class = F8&nbsp;V<ref name=SIMBAD/>
| class = F8&nbsp;V<ref name=SIMBAD/>
| u-b = –0.01<ref name=clpl4_99/>
| u-b = −0.01<ref name=clpl4_99/>
| b-v = +0.52<ref name=clpl4_99/>
| b-v = +0.52<ref name=clpl4_99/>
| r-i =
| r-i =
| component2 = B
| type2 = [[main sequence]]
| class2 = K7Ve<ref name=ds2018/>
| u-b2 =
| b-v2 = +1.34<ref name=borosaikia2018/>
| r-i2 =
}}
}}
{{Starbox astrometry
{{Starbox astrometry
| component1 = A
⚫
| radial_v = +8.5<ref name=aaa418_989/>
| prop_mo_ra = –176.71<ref name=aaa474_2_653/>
| radial_v = +8.57<ref name=dr3a/>
| prop_mo_dec = –33.21<ref name=aaa474_2_653/>
| prop_mo_ra = −177.045<ref name=dr3a/>
| prop_mo_dec = −32.634<ref name=dr3a/>
| parallax = 78.25
| p_error = 0.28
| parallax = 77.2485
| p_error = 0.0805
| parallax_footnote = <ref name=aaa474_2_653/>
| parallax_footnote = <ref name=dr3a/>
| absmag_v = 4.29<ref name=aaa418_989/>
| absmag_v = 4.29<ref name=aaa418_989/>
| component2 = B
| radial_v2 = +8.67<ref name=dr3b/>
| prop_mo_ra2 = −182.443<ref name=dr3b/>
| prop_mo_dec2 = −32.034<ref name=dr3a/>
| parallax2 = 77.4072
| p_error2 = 0.0182
| parallax_footnote2 = <ref name=dr3b/>
| absmag_v2 = 8.2<ref name=borosaikia2018/>
}}
}}
{{Starbox detail
{{Starbox detail
| component1 = A
⚫
| mass = 1.121<ref name=apjss168_2_297/>
| radius = {{nowrap|1.091 ± 0.020}}<ref name=apj746_1_101/>
| mass = 1.10<ref name=dr3a/>
| gravity = 4.36<ref name=aaas141_491/>
| radius = 1.17<ref name=dr3a/>
| metal_fe = –0.18<ref name=aaas141_491/>
| gravity = 4.4.23<ref name=dr3a/>
| age_gyr = 2.7<ref name=aaa418_989/>
| metal_fe = −0.09<ref name=chavero2021/>
| temperature = {{nowrap|6,233 ± 68}}<ref name=apj746_1_101/>
| age_gyr = 4.0<ref name=dr3a/>
| luminosity = {{nowrap|1.605 ± 0.042}}<ref name=apj746_1_101/>
| temperature = 6,066<ref name=dr3a/>
| rotational_velocity = 5.5<ref name=aaa493_3_1099/>
| luminosity = 1.69<ref name=dr3a/>
| rotational_velocity = 1.50<ref name=chavero2021/>
| component2 = B
| mass2 = 0.626<ref name=ticv8/>
| radius2 = 0.648<ref name=ticv8/>
| gravity2 = 4.61<ref name=ticv8/>
| metal_fe2 = −0.08<ref name=gaidos2014/>
| age_gyr2 = 5<ref name=ry2019/>
| temperature2 = 4,132<ref name=gaidos2014/>
| luminosity2 = 0.10<ref name=gaidos2014/>
| rotational_velocity2 = 9<ref name=lv2019/>
}}
}}
{{Starbox catalog
{{Starbox catalog
Line 44: Line 76:
{{Starbox end}}
{{Starbox end}}


'''36 Ursae Majoris''' is a [[double star]]<ref name=SIMBAD/> in the northern constellation of [[Ursa Major]]. With an [[apparent visual magnitude]] of 4.82,<ref name=clpl4_99/> it can be seen with the naked eye in [[Bortle Dark-Sky Scale|suitable dark skies]]. Based upon [[parallax]] measurements, this star lies at a distance of {{Convert|41.7|ly|pc|abbr=off|lk=on}} from [[Earth]].<ref name=aaa474_2_653/>
'''36 Ursae Majoris''' is a [[double star]]<ref name=SIMBAD/> in the northern constellation of [[Ursa Major]]. With an [[apparent visual magnitude]] of 4.8, it can be seen with the naked eye in [[Bortle Dark-Sky Scale|suitable dark skies]]. Based upon [[parallax]] measurements, this binary lies at a distance of {{Convert|42|ly|pc|abbr=off|lk=on}} from [[Earth]].


This star is a [[solar analog]]—meaning it has physical properties that make it similar to the Sun. It has 12% more mass and a radius 15% larger than the Sun,<ref name=apjss168_2_297/> with an estimated age of 2.7 billion years.<ref name=aaa418_989/> The [[stellar spectrum|spectrum]] of this star matches a [[stellar classification]] of F8&nbsp;V, which indicates this is a [[main sequence]] star that is generating energy at its core through the [[nuclear fusion]] of hydrogen. The energy is being radiated into space from its outer envelope at an [[effective temperature]] of 6,126&nbsp;K.<ref name=apj159_1_141/> This gives the star the characteristic yellow-white hue of an F-type star.<ref name=csiro/>
This star is a [[solar analog]]—meaning it has physical properties that make it similar to the Sun. It has 12% more mass and a radius 15% larger than the Sun,<ref name=apjss168_2_297/> with an estimated age of 2.7 billion years.<ref name=aaa418_989/> The [[stellar spectrum|spectrum]] of this star matches a [[stellar classification]] of F8&nbsp;V, which indicates this is a [[main sequence]] star that is generating energy at its core through the [[nuclear fusion]] of hydrogen. The energy is being radiated into space from its outer envelope at an [[effective temperature]] of 6,126&nbsp;K.<ref name=apj159_1_141/> This gives the star the characteristic yellow-white hue of an F-type star.<ref name=csiro/>
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{{reflist|30em|refs=
{{reflist|30em|refs=


<ref name=dr3a>{{cite Gaia DR3|853819947756949120}}</ref>
<ref name=aaa474_2_653>{{citation | first1=F. | last1=van Leeuwen |date=November 2007 | title=Validation of the new Hipparcos reduction | journal=Astronomy and Astrophysics | volume=474 | issue=2 | pages=653–664 | bibcode=2007A&A...474..653V | doi=10.1051/0004-6361:20078357 |arxiv = 0708.1752 | s2cid=18759600 }}</ref>


<ref name=dr3b>{{cite Gaia DR3|853820948481913472}}</ref>
⚫
<ref name=aaas141_491>{{citation | display-authors=1 | last1=Chen | first1=Y. Q. | last2=Nissen | first2=P. E. | last3=Zhao | first3=G. | last4=Zhang | first4=H. W. | last5=Benoni | first5=T. | title=Chemical composition of 90 F and G disk dwarfs | journal=Astronomy and Astrophysics Supplement | volume=141 | pages=491–506 | doi=10.1051/aas:2000124 | bibcode=2000A&AS..141..491C |arxiv = astro-ph/9912342 |date=February 2000| issue=3 | s2cid=16273589 }}</ref>


<ref name=apj159_1_141>{{citation | author=Valenti, Jeff A. | author2=Fischer, Debra A. | title=Spectroscopic Properties of Cool Stars (SPOCS). I. 1040 F, G, and K Dwarfs from Keck, Lick, and AAT Planet Search Programs | journal=The Astrophysical Journal Supplement Series | volume=159 | issue=1 | pages=141–166 | doi=10.1086/430500 | bibcode=2005ApJS..159..141V |date=July 2005| doi-access=free }}</ref>
<ref name=apj159_1_141>{{citation | author=Valenti, Jeff A. | author2=Fischer, Debra A. | title=Spectroscopic Properties of Cool Stars (SPOCS). I. 1040 F, G, and K Dwarfs from Keck, Lick, and AAT Planet Search Programs | journal=The Astrophysical Journal Supplement Series | volume=159 | issue=1 | pages=141–166 | doi=10.1086/430500 | bibcode=2005ApJS..159..141V |date=July 2005| doi-access=free }}</ref>


<ref name=aaa418_989>{{citation | display-authors=1 | last1=Nordström | first1=B. | last2=Mayor | first2=M. | last3=Andersen | first3=J. | last4=Holmberg | first4=J. | last5=Pont | first5=F. | last6=Jørgensen | first6=B. R. | last7=Olsen | first7=E. H. | last8=Udry | first8=S. | last9=Mowlavi | first9=N. | title=The Geneva-Copenhagen survey of the Solar neighbourhood. Ages, metallicities, and kinematic properties of ˜14 000 F and G dwarfs | journal=Astronomy and Astrophysics | volume=418 | pages=989–1019 | doi=10.1051/0004-6361:20035959 | bibcode=2004A&A...418..989N| issue=3 | arxiv=astro-ph/0405198 |date=May 2004| s2cid=11027621 }}</ref>
<ref name=aaa418_989>{{citation | display-authors=1 | last1=Nordström | first1=B. | last2=Mayor | first2=M. | last3=Andersen | first3=J. | last4=Holmberg | first4=J. | last5=Pont | first5=F. | last6=Jørgensen | first6=B. R. | last7=Olsen | first7=E. H. | last8=Udry | first8=S. | last9=Mowlavi | first9=N. | title=The Geneva-Copenhagen survey of the Solar neighbourhood. Ages, metallicities, and kinematic properties of ˜14 000 F and G dwarfs | journal=Astronomy and Astrophysics | volume=418 | pages=989–1019 | doi=10.1051/0004-6361:20035959 | bibcode=2004A&A...418..989N| issue=3 | arxiv=astro-ph/0405198 |date=May 2004| s2cid=11027621 }}</ref>

<ref name=aaa493_3_1099>{{citation | last1=Schröder | first1=C. | last2=Reiners | first2=Ansgar | last3=Schmitt | first3=Jürgen H. M. M. | title=Ca II HK emission in rapidly rotating stars. Evidence for an onset of the solar-type dynamo | journal=Astronomy and Astrophysics | volume=493 | issue=3 | pages=1099–1107 | date=January 2009 | doi=10.1051/0004-6361:200810377 | bibcode=2009A&A...493.1099S | doi-access=free | url=http://goedoc.uni-goettingen.de/goescholar/bitstream/handle/1/9690/aa10377-08.pdf?sequence=2 }}</ref>


<ref name=clpl4_99>{{citation | display-authors=1 | last1=Johnson | first1=H. L. | last2=Iriarte | first2=B. | last3=Mitchell | first3=R. I. | last4=Wisniewskj | first4=W. Z. | title=UBVRIJKL photometry of the bright stars | journal=Communications of the Lunar and Planetary Laboratory | volume=4 | issue=99 | date=1966 | page=99 | bibcode=1966CoLPL...4...99J }}</ref>
<ref name=clpl4_99>{{citation | display-authors=1 | last1=Johnson | first1=H. L. | last2=Iriarte | first2=B. | last3=Mitchell | first3=R. I. | last4=Wisniewskj | first4=W. Z. | title=UBVRIJKL photometry of the bright stars | journal=Communications of the Lunar and Planetary Laboratory | volume=4 | issue=99 | date=1966 | page=99 | bibcode=1966CoLPL...4...99J }}</ref>
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<ref name=csiro>{{citation|title=The Colour of Stars |date=December 21, 2004 |work=Australia Telescope, Outreach and Education |publisher=[[Commonwealth Scientific and Industrial Research Organisation]] |url=http://outreach.atnf.csiro.au/education/senior/astrophysics/photometry_colour.html |access-date=2012-01-16 |url-status=dead |archive-url=https://web.archive.org/web/20120318151427/http://outreach.atnf.csiro.au/education/senior/astrophysics/photometry_colour.html |archive-date=March 18, 2012 }}</ref>
<ref name=csiro>{{citation|title=The Colour of Stars |date=December 21, 2004 |work=Australia Telescope, Outreach and Education |publisher=[[Commonwealth Scientific and Industrial Research Organisation]] |url=http://outreach.atnf.csiro.au/education/senior/astrophysics/photometry_colour.html |access-date=2012-01-16 |url-status=dead |archive-url=https://web.archive.org/web/20120318151427/http://outreach.atnf.csiro.au/education/senior/astrophysics/photometry_colour.html |archive-date=March 18, 2012 }}</ref>

<ref name=apj746_1_101>{{citation | display-authors=1 | last1=Boyajian | first1=Tabetha S. | last2=McAlister | first2=Harold A. | last3=van Belle | first3=Gerard | last4=Gies | first4=Douglas R. | last5=ten Brummelaar | first5=Theo A. | last6=von Braun | first6=Kaspar | last7=Farrington | first7=Chris | last8=Goldfinger | first8=P. J. | last9=O'Brien | first9=David | last10=Parks | first10=J. Robert | last11=Richardson | first11=Noel D. | last12=Ridgway | first12=Stephen | last13=Schaefer | first13=Gail | last14=Sturmann | first14=Laszlo | last15=Sturmann | first15=Judit | last16=Touhami | first16=Yamina | last17=Turner | first17=Nils H. | last18=White | first18=Russel | title=Stellar Diameters and Temperatures. I. Main-sequence A, F, and G Stars | journal=The Astrophysical Journal | volume=746 | issue=1 | page=101 | doi=10.1088/0004-637X/746/1/101 | bibcode=2012ApJ...746..101B |arxiv = 1112.3316 |date=February 2012| s2cid=18993744 }}. See Table 10.</ref>


<ref name=aa555_A11>{{cite journal
<ref name=aa555_A11>{{cite journal
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|doi = 10.1086/323920 | doi-access=free
|doi = 10.1086/323920 | doi-access=free
}}</ref>
}}</ref>

<ref name=ds2018>{{citation
| title=The Penn State - Toruń Centre for Astronomy Planet Search stars. IV. Dwarfs and the complete sample
| last1=Deka-Szymankiewicz | first1=B. | last2=Niedzielski | first2=A.
| last3=Adamczyk | first3=M. | last4=Adamów | first4=M.
| last5=Nowak | first5=G. | last6=Wolszczan | first6=A.
| display-authors=1 | journal=Astronomy and Astrophysics
| volume=615 | pages=A31 | year=2018 | postscript=.
| arxiv=1801.02899 | bibcode=2018A&A...615A..31D
| doi=10.1051/0004-6361/201731696 | s2cid=85526201 }}</ref>

<ref name=borosaikia2018>{{citation
| last1=Boro Saikia |first1=S. |last2=Marvin |first2=C. J.
| last3=Jeffers |first3=S. V. |last4=Reiners |first4=Ansgar
| last5=Cameron |first5=R. |last6=Marsden |first6=S. C.
| last7=Petit |first7=P. |last8=Warnecke |first8=J.
| last9=Yadav |first9=A. P. |last10=Teske |first10=J. K.
| last11=Shectman |first11=S. A. |last12=Crane |first12=J. D.
| last13=Thompson |first13=I. |last14=Keiser |first14=S.
| last15=Jenkins |first15=J. S. |last16=Berdiñas |first16=Z.
| last17=Diaz |first17=M. |last18=Kiraga |first18=M.
| last19=Barnes |first19=J. R. |display-authors=1
| title=Chromospheric activity catalogue of 4454 cool stars. Questioning the active branch of stellar activity cycles
| journal=Astronomy and Astrophysics
| volume=616 | pages=A108 | year=2018
| bibcode=2018A&A...616A.108B | arxiv=1803.11123
| doi=10.1051/0004-6361/201629518 | s2cid=118915212 | postscript=. }}</ref>

<ref name=ticv8>{{citation |postscript=. | display-authors = 1 | last1 = Stassun | first1 = Keivan G. | last2 = Oelkers | first2 = Ryan J. | last3 = Paegert | first3 = Martin | last4 = Torres | first4 = Guillermo | last5 = Pepper | first5 = Joshua | last6 = Lee | first6 = Nathan De | last7 = Collins | first7 = Kevin | last8 = Latham | first8 = David W. | last9 = Muirhead | first9 = Philip S. | last10 = Chittidi | first10 = Jay | last11 = Rojas-Ayala | first11 = Bárbara | last12 = Fleming | first12 = Scott W. | last13 = Rose | first13 = Mark E. | last14 = Tenenbaum | first14 = Peter | last15 = Ting | first15 = Eric B. | last16 = Kane | first16 = Stephen R. | last17 = Barclay | first17 = Thomas | last18 = Bean | first18 = Jacob L. | last19 = Brassuer | first19 = C. E. | last20 = Charbonneau | first20 = David | last21 = Ge | first21 = Jian | last22 = Lissauer | first22 = Jack J. | last23 = Mann | first23 = Andrew W. | last24 = McLean | first24 = Brian | last25 = Mullally | first25 = Susan | last26 = Narita | first26 = Norio | last27 = Plavchan | first27 = Peter | last28 = Ricker | first28 = George R. | last29 = Sasselov | first29 = Dimitar | last30 = Seager | first30 = S. | last31 = Sharma | first31 = Sanjib | last32 = Shiao | first32 = Bernie | last33 = Sozzetti | first33 = Alessandro | last34 = Stello | first34 = Dennis | last35 = Vanderspek | first35 = Roland | last36 = Wallace | first36 = Geoff | last37 = Winn | first37 = Joshua N. | title = The Revised ''TESS'' Input Catalog and Candidate Target List | journal = The Astronomical Journal | date = 9 September 2019 | volume = 158 | issue = 4 | page = 138 | eissn = 1538-3881 | doi = 10.3847/1538-3881/ab3467 | bibcode = 2019AJ....158..138S | arxiv = 1905.10694 | doi-access = free}}</ref>

<ref name=gaidos2014>{{citation |postscript=.
| title=M dwarf metallicities and giant planet occurrence: ironing out uncertainties and systematics
| last1=Gaidos | first1=Eric | last2=Mann | first2=Andrew W.
| journal=The Astrophysical Journal | arxiv=1406.4071
| volume=791 | issue=1 | id=54 | pages=9 | date=August 2014
| doi=10.1088/0004-637X/791/1/54 | bibcode=2014ApJ...791...54G | s2cid=118744016 }}</ref>

<ref name=ry2019>{{citation |postscript=. |bibcode=2019ApJ...872...17R |title=HAZMAT. V. The Ultraviolet and X-Ray Evolution of K Stars |last1=Richey-Yowell |first1=Tyler |last2=Shkolnik |first2=Evgenya L. |last3=Schneider |first3=Adam C. |last4=Osby |first4=Ella |last5=Barman |first5=Travis |last6=Meadows |first6=Victoria S. |journal=The Astrophysical Journal |year=2019 |volume=872 |issue=1 |page=17 |doi=10.3847/1538-4357/aafa74 |arxiv=1901.00502 |s2cid=119423234 }}</ref>

<ref name=lv2019>{{citation |postscript=. |bibcode=2019ApJ...879..105L |title=Effective Temperatures of Low-mass Stars from High-resolution H-band Spectroscopy |last1=López-Valdivia |first1=Ricardo |last2=Mace |first2=Gregory N. |last3=Sokal |first3=Kimberly R. |last4=Hussaini |first4=Maryam |last5=Kidder |first5=Benjamin T. |last6=Mann |first6=Andrew W. |last7=Gosnell |first7=Natalie M. |last8=Oh |first8=Heeyoung |last9=Kesseli |first9=Aurora Y. |last10=Muirhead |first10=Philip S. |last11=Johns-Krull |first11=Christopher M. |last12=Jaffe |first12=Daniel T. |journal=The Astrophysical Journal |year=2019 |volume=879 |issue=2 |page=105 |doi=10.3847/1538-4357/ab2129 |arxiv=1905.05076 |s2cid=152282781 }}</ref>

⚫
<ref name=chavero2021>{{citation |postscript=. | last1 = Llorente de Andrés | first1 = F. | last2 = Chavero | first2 = C. | last3 = de la Reza | first3 = R. | last4 = Roca-Fàbrega | first4 = S. | last5 = Cifuentes | first5 = C. | title = The evolution of lithium in FGK dwarf stars | journal = Astronomy & Astrophysics | date = October 2021 | volume = 654 | page = A137 | issn = 0004-6361 | eissn = 1432-0746 | doi = 10.1051/0004-6361/202141339 | bibcode = 2021A&A...654A.137L | arxiv = 2108.05852 | doi-access = free}}</ref>


}}
}}

Revision as of 14:34, 13 October 2022

36 Ursae Majoris
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Ursa Major
A
Right ascension 10h 30m 37.5793s[1]
Declination +55° 58′ 49.940″[1]
Apparent magnitude (V) 4.82[2]
B
Right ascension 10h 30m 25.3089s[3]
Declination +55° 59′ 56.855″[3]
Apparent magnitude (V) 8.86[4]
Characteristics
A
Evolutionary stage main sequence
Spectral type F8 V[5]
U−B color index −0.01[2]
B−V color index +0.52[2]
B
Evolutionary stage main sequence
Spectral type K7Ve[6]
B−V color index +1.34[7]
Astrometry
A
Radial velocity (Rv)+8.57[1] km/s
Proper motion (μ) RA: −177.045[1] mas/yr
Dec.: −32.634[1] mas/yr
Parallax (π)77.2485 ± 0.0805 mas[1]
Distance42.22 ± 0.04 ly
(12.95 ± 0.01 pc)
Absolute magnitude (MV)4.29[8]
B
Radial velocity (Rv)+8.67[3] km/s
Proper motion (μ) RA: −182.443[3] mas/yr
Dec.: −32.034[1] mas/yr
Parallax (π)77.4072 ± 0.0182 mas[3]
Distance42.135 ± 0.010 ly
(12.919 ± 0.003 pc)
Absolute magnitude (MV)8.2[7]
Details
A
Mass1.10[1] M☉
Radius1.17[1] R☉
Luminosity1.69[1] L☉
Surface gravity (log g)4.4.23[1] cgs
Temperature6,066[1] K
Metallicity [Fe/H]−0.09[9] dex
Rotational velocity (v sin i)1.50[9] km/s
Age4.0[1] Gyr
B
Mass0.626[4] M☉
Radius0.648[4] R☉
Luminosity0.10[10] L☉
Surface gravity (log g)4.61[4] cgs
Temperature4,132[10] K
Metallicity [Fe/H]−0.08[10] dex
Rotational velocity (v sin i)9[11] km/s
Age5[12] Gyr
Other designations
36 Ursae Majoris, BD+56 1459, FK5 394, HD 90839, HIP 51459, HR 4112, SAO 27670.[5]
Database references
SIMBADA
B

36 Ursae Majoris is a double star[5] in the northern constellation of Ursa Major. With an apparent visual magnitude of 4.8, it can be seen with the naked eye in suitable dark skies. Based upon parallax measurements, this binary lies at a distance of 42 light-years (13 parsecs) from Earth.

This star is a solar analog—meaning it has physical properties that make it similar to the Sun. It has 12% more mass and a radius 15% larger than the Sun,[13] with an estimated age of 2.7 billion years.[8] The spectrum of this star matches a stellar classification of F8 V, which indicates this is a main sequence star that is generating energy at its core through the nuclear fusion of hydrogen. The energy is being radiated into space from its outer envelope at an effective temperature of 6,126 K.[14] This gives the star the characteristic yellow-white hue of an F-type star.[15]

36 Ursae Majoris has a magnitude 8.86 common proper motion companion with about half this star's mass[16] at an angular separation of 122.5″ along a position angle of 303°, as of 2012. A second companion with a magnitude of 11.44 is located at an angular separation of 240.6″ along a position angle of 292°, as of 2004.[17]

Hunt for substellar objects

According to Nelson & Angel (1998),[18] 36 Ursae Majoris could host one or two (or at least three) jovian planets (or even brown dwarfs) at wide separations from the host star, with orbital periods of 10–15, 25 and 50 years respectively. The authors have set upper limits of 1.1–2, 5.3 and 24 Jupiter masses for the putative planetary objects. Also Lippincott (1983)[19] had previously noticed the possible presence of a massive unseen companion (with nearly 70 times the mass of Jupiter, just below the stellar regime, thus a brown dwarf). Putative parameters for the substellar object show an orbital period of 18 years and quite a high eccentricity (e=0.8). Even Campbell et al. 1988[20] inferred the existence of planetary objects or even brown dwarfs less massive than 14 Jupiter masses around 36 Ursae Majoris.

Nevertheless, no certain planetary companion has yet been detected or confirmed. The McDonald Observatory team has set limits to the presence of one or more planets[21] with masses between 0.13 and 2.5 Jupiter masses and average separations spanning between 0.05 and 5.2 AU.

An infrared excess has been detected around this star, most likely indicating the presence of a circumstellar disk at a radius of 38.6 AU. The temperature of this dust is 50 K.[22]

References

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  18. ^ The Range of Masses and Periods Explored by Radial Velocity Searches for Planetary Companions
  19. ^ An unseen companion to 36 Ursae Majoris A from analysis of plates taken with the Sproul 61-CM refractor
  20. ^ A search for substellar companions to southern solar-type stars
  21. ^ Detection Limits from the McDonald Observatory Planet Search Program
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External links

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