| 词条 | V429 Geminorum |
| 释义 |
| name = BD+20° 1790 }}{{Starbox observe | epoch = J2000.0 | constell = Gemini | ra = {{RA|07|23|43.592}} | dec = {{DEC|+20|24|58.66}} | appmag_v = 9.93 }}{{Starbox character | class = K5Ve[1] | appmag_1_passband = B | appmag_1 = 11.08 | appmag_2_passband = R | appmag_2 = 9.43 | appmag_3_passband = I | appmag_3 = 8.9 | appmag_4_passband = J | appmag_4 = 7.643 | appmag_5_passband = H | appmag_5 = 7.032 | appmag_6_passband = K | appmag_6 = 6.879 | b-v = 1.15 | v-r = 0.50 | r-i = 0.5 | variable = BY Dra[2] }}{{Starbox astrometry | radial_v = +9.3 | prop_mo_ra = −65.8 | prop_mo_dec = −228.1 | dist_ly = 84.76 | dist_pc = 26[1] | absmag_v = 7.86 }}{{Starbox detail | mass = 0.63[4] | radius = 0.71[4] | gravity = 4.53[4] | luminosity = 0.17[4] | temperature = 4410[4] | metal = 0.30[4] | age = 35-80[4][3]million | rotation = 3.59 days | rotational_velocity = 10.03[4] }}{{Starbox catalog | names = V429 Gem, BD+20°1790, TYC 1355-214-1, USNO-B1.0 1104-00142035, 2MASS J07234358+2024588, 1SWASP J072343.59+202458.6 }}{{Starbox reference | Simbad = BD%2B20+1790 | NSTED = BD%2B20+1790 | EPE = BD%2B20+1790 }}{{Starbox end}} V429 Geminorum (BD+20°1790) is a young orange dwarf star in the constellation Gemini, located nearly 85 light years away from the Sun. It is a BY Draconis variable, a cool dwarf which varies rapidly in brightness as it rotates. DescriptionThe star is young and very active and is a member of the AB Doradus Moving Group.[4] The star has also been studied and monitored by SuperWASP group and found to coincide with the ROSAT source 1RXS J072343.6+202500.[5] The planet candidate was announced in December 2009.[4] Disproven planetThe Keplerian fit of the RV data suggested an orbital solution for a close-in massive planet with an orbital period of 7.7834 days. Moreover, the presence of a close-in massive jovian planet could explain the high level of stellar activity detected.[6] However, further study suggests that this planet may not exist because the radial velocity variations are strongly correlated to stellar activity, suggesting this activity is the cause of the variations.[7] This echoes the similar case of the disproven planet detection around TW Hydrae, which was also found to be due to stellar activity rather than orbital motion.[8] References1. ^1 {{cite journal | arxiv=0808.3362| author=Torres & Quast | author2=Quast, G. R. | author3=Melo, C. H. F. | author4=Sterzik, M. F. | title=Young Nearby Loose Associations| journal=Handbook of Star Forming Regions, Volume II: the Southern Sky ASP Monograph Publications | volume=5| pages=1–757| year=2008 | bibcode=2008hsf2.book..757T}} 2. ^{{cite journal|bibcode=2009yCat....102025S|title=VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)|journal=VizieR On-line Data Catalog: B/gcvs. Originally published in: 2009yCat....102025S|volume=1|display-authors=etal|author1=Samus|first1=N. N.|last2=Durlevich|first2=O. V.|year=2009}} 3. ^{{cite journal | arxiv=0810.1003| author=Carpenter | author2=Bouwman, Jeroen | author3=Mamajek, Eric E. | author4=Meyer, Michael R. | author5=Hillenbrand, Lynne A. | author6=Backman, Dana E. | author7=Henning, Thomas | author8=Hines, Dean C. | author9=Hollenbach, David| title=Formation and Evolution of Planetary Systems: Properties of Debris Dust Around Solar-Type Stars| journal=The Astrophysical Journal Supplement | volume=181| issue=1| pages=197–226| year=2009 | doi=10.1088/0067-0049/181/1/197 | bibcode=2009ApJS..181..197C| display-authors=8 | last10=Kim | first10=Jinyoung Serena | last11=Moro-Martin | first11=Amaya | last12=Pascucci | first12=Ilaria | last13=Silverstone | first13=Murray D. | last14=Stauffer | first14=John R. | last15=Wolf | first15=Sebastian }} 4. ^{{cite journal | arxiv=astro-ph/0601573| author=Lopez-Santiago | author2=Montes, D. | author3=Crespo-Chacón, I. | author4=Fernández-Figueroa, M. J. | title=The Nearest Young Moving Groups| journal=The Astrophysical Journal | volume=643| issue=2|pages=1160–1165| year=2006 | doi=10.1086/503183 | bibcode=2006ApJ...643.1160L|display-authors=etal}} 5. ^{{cite journal | doi=10.1051/0004-6361:20077084 | arxiv=astro-ph/0702631| author=Norton | last2=Wheatley | first2=P. J. | last3=West | first3=R. G. | last4=Haswell | first4=C. A. | last5=Street | first5=R. A. | last6=Collier Cameron | first6=A. | last7=Christian | first7=D. J. | last8=Clarkson | first8=W. I. | last9=Enoch | first9=B. | last10=Gallaway| first10=M.| last11=Hellier| first11=C.| last12=Horne| first12=K.| last13=Irwin| first13=J.| last14=Kane| first14=S. R.| last15=Lister| first15=T. A.| last16=Nicholas| first16=J. P.| last17=Parley| first17=N.| last18=Pollacco| first18=D.| last19=Ryans| first19=R.| last20=Skillen| first20=I.| last21=Wilson| first21=D. M.| title=New periodic variable stars coincident with ROSAT sources discovered using SuperWASP| journal=Astronomy and Astrophysics | volume=467| issue=2|pages=785–905| year=2007 | bibcode=2007A&A...467..785N| display-authors=8}} 6. ^1 2 3 4 5 6 7 8 9 {{Cite journal| arxiv=0912.2773 | author=Hernán-Obispo | author2=Gálvez-Ortiz, M. C. | author3=Anglada-Escudé, G. | author4=Kane, S. R. | author5=Barnes, J. R. | author6=de Castro, E. | author7=Cornide, M. | title=Evidence of a massive planet candidate orbiting the young active K5V star BD+20 1790 | journal=Astronomy and Astrophysics | volume=0912| pages=A45 | year=2009 |display-authors=etal| doi=10.1051/0004-6361/200811000 |bibcode = 2010A&A...512A..45H }} 7. ^{{Cite journal|arxiv=1003.3678|title=Evidence against the young hot-Jupiter around BD +20 1790|journal=Astronomy and Astrophysics|volume=513|pages=L8|author=Figueira|year=2010|author2=Marmier|author3=Bonfils|author4=di Folco|author5=Udry|author6=Santos|author7=Lovis|author8=Megevand|author9=Melo|last10= Pepe|first10=F.|last11= Queloz|first11=D.|last12= Segransan|first12=D.|last13= Triaud|first13=A. H. M. J.|last14= Viana Almeida|first14=P.|display-authors=etal|doi=10.1051/0004-6361/201014323|bibcode = 2010A&A...513L...8F }} 8. ^{{cite journal|url=http://www.aanda.org/index.php?option=article&access=standard&Itemid=129&url=/articles/aa/abs/2008/38/aa10596-08/aa10596-08.html|author=Huelamo, N.|title=TW Hydrae: evidence of stellar spots instead of a Hot Jupiter|journal=Astronomy and Astrophysics|volume=489|issue=2|pages=L9–L13|year=2008|accessdate=2008-10-02|doi=10.1051/0004-6361:200810596|bibcode=2008A&A...489L...9H|arxiv = 0808.2386 |last2=Figueira|first2=P.|last3=Bonfils|first3=X.|last4=Santos|first4=N. C.|last5=Pepe|first5=F.|last6=Gillon|first6=M.|last7=Azevedo|first7=R.|last8=Barman|first8=T.|last9=Fernández|first9=M.|last10=Di Folco|first10=E.|last11=Guenther|first11=E. W.|last12=Lovis|first12=C.|last13=Melo|first13=C. H. F.|last14=Queloz|first14=D.|last15=Udry|first15=S.|display-authors=etal}} See also
6 : K-type main-sequence stars|Gemini (constellation)|Durchmusterung objects|Hypothetical planetary systems|Objects with variable star designations|BY Draconis variables |
| 随便看 |
|
开放百科全书收录14589846条英语、德语、日语等多语种百科知识，基本涵盖了大多数领域的百科知识，是一部内容自由、开放的电子版国际百科全书。