编辑“︁HD 13445”︁（章节）

== 成員星 ==
該聯星系統的主星（HD 13445 A、Gliese 86 A）是一顆[[恆星光譜|光譜類型]] K1V 的[[橙矮星]]，質量是太陽的79%，半徑則是太陽的0.86倍，光度則是太陽的35%。該恆星旁有一顆距離相當近的類木行星

伴星 HD 13445 B（Gliese 86 B）是一顆白矮星，距離主星約21天文單位，因此讓該聯星系統成為擁有系外行星的聯星中結構最緊密的系統之一<ref>{{cite journal | url=http://www.iop.org/EJ/article/0004-637X/646/1/523/64035.html | title=Two Suns in The Sky: Stellar Multiplicity in Exoplanet Systems | author=Raghavan |display-authors=etal | journal=The [[Astrophysical Journal]] | volume=646 | issue=1 | pages=523–542 | year=2006 | doi=10.1086/504823 | last2=Henry | first2=Todd J. | last3=Mason | first3=Brian D. | last4=Subasavage | first4=John P. | last5=Jao | first5=Wei‐Chun | last6=Beaulieu | first6=Thom D. | last7=Hambly | first7=Nigel C. | bibcode=2006ApJ...646..523R | arxiv=astro-ph/0603836 | access-date=2013-03-26 | archive-date=2020-04-28 | archive-url=https://web.archive.org/web/20200428162417/https://hkvalidate.perfdrive.com/captcha?ssa=1ba0b55e-0b1b-4271-8dc3-16486b421f08&ssb=za2z2m6f2adih2m541gai0c5h&ssc=http%3A%2F%2Fiopscience.iop.org%2Farticle%2F0004-637X%2F646%2F1%2F523%2F64035.html&ssd=463308223507856&sse=adb%40jciedbcleel&ssf=cabbbe92ac3fea603c4b236ce0d026e2a3a7dc24&ssg=603d6e36-3553-4bbe-a751-8be11a318fa7&ssh=cf9a8d8a-c6ab-4ba5-881e-8bda531f1e6c&ssi=193c4e08-8427-4a68-9b82-6c95a701fad8&ssj=9e871f84-d77d-4a17-97fc-901e35c24f6e&ssk=support%40shieldsquare.com&ssl=040603155946&ssm=42544857964150236107565674411659&ssn=7b26e3023f13e17498682021a6d87ba4f295192fc894-bdd8-4a27-9918e9&sso=987691c9-760ce8b2495e594392fdb2bdf1577489429cad276e99f8d4&ssp=16246728041588005526158807818302904&ssq=40203459105690637448291056473541058707772&ssr=MjA3LjI0MS4yMjYuMjMw&sss=Chrome%2F5.0%20%28iPhone%3B%20U%3B%20CPU%20iPhone%20OS%203_0%20like%20Mac%20OS%20X%3B%20en-us%29%20AppleWebKit%2F528.18%20%28KHTML%2C%20like%20Gecko%29%20Version%2F4.0%20Mobile%2F7A341%20Safari%2F528.16&sst=python-requests%2F2.23.0&ssu=Mozilla%2F5.0%20%28compatible%3B%20Googlebot%2F2.1%3B%20+http%3A%2F%2Fwww.google.com%2Fbot.html%29&ssv=p%40r3lrv11vrt%404%40&ssw=&ssx=775604223893518&ssy=mmgmgnhmafbk%40lgbibelaogjlbdl%40hhjllgjnlen&ssz=647afc3a18dc228 | dead-url=no }}</ref>。該白矮星發現於2001年，原被認為是[[棕矮星]]<ref>{{cite journal | url=http://www.aanda.org/articles/aa/full/2001/16/aadb012/aadb012.html | title=A second substellar companion in the Gliese 86 system. A brown dwarf in an extrasolar planetary system | author=Els, S. G. |display-authors=etal | journal=[[Astronomy and Astrophysics]] | volume=370 | issue=1 | pages=L1–L4 | year=2001 | doi=10.1051/0004-6361:20010298 | bibcode=2001A&A...370L...1E | access-date=2013-03-26 | archive-date=2019-06-26 | archive-url=https://web.archive.org/web/20190626032216/https://www.aanda.org/articles/aa/full/2001/16/aadb012/aadb012.html | dead-url=no }}</ref>，但在2005年的觀測結果中顯示它是白矮星，因為它的光譜並沒有代表棕矮星特徵的分子吸收線<ref>{{cite journal |bibcode=2005MNRAS.361L..15M |title=Gl86B: a white dwarf orbits an exoplanet host star|author=Mugrauer, M. and Neuhäuser, R.|journal=[[Monthly Notices of the Royal Astronomical Society|Monthly Notices of the Royal Astronomical Society: Letters]]|volume=361|issue=1|pages=L15–L19|year=2005|doi=10.1111/j.1745-3933.2005.00055.x|arxiv = astro-ph/0506311 }}</ref>。假設該白矮星的質量大約是太陽的一半，並且徑向速度觀測的線性趨勢是因為這顆伴星，它環繞主星的軌道半長軸可能是18.42天文單位，並且[[軌道離心率]]是0.3974<ref>{{cite journal |bibcode=2006A&A...459..955L |title=New constrains on Gliese 86 B. VLT near infrared coronographic imaging survey of planetary hosts|author=Lagrange, A.-M. |display-authors=etal |journal=[[Astronomy and Astrophysics]]|volume=459|issue=3|pages=955–963|year=2006|doi=10.1051/0004-6361:20054710}}</ref>。