사용자:Ta183ta/연습장: 두 판 사이의 차이

The secondary, now more massive star is surrounded by an [[accretion disk]] from this mass transfer, with [[bipolar jets|bipolar, jet-like features]] projecting perpendicular to the disk.<ref name=apj684_2_L95/> This accretion disk blocks humans' view of the secondary star, lowering its apparent luminosity and making it difficult for astronomers to pinpoint what its stellar type is. The amount of mass being transferred between the two stars is about {{nowrap|2 × 10⁻⁵ }}[[solar mass]]es per year, or the equivalent of the Sun's mass every 50,000 years, which results in an increase in orbital period of about 19 seconds each year. The [[stellar spectrum|spectrum]] of Beta Lyrae shows emission lines produced by the accretion disc. The disc produces around 20% of the brightness of the system.<ref name=apj684_2_L95/>

 

 

The two components are so close together that they cannot be resolved with optical telescopes, forming a [[spectroscopic binary]]. In 2008, the primary star and the accretion disk of the secondary star were resolved and imaged using the [[CHARA array|CHARA Array]] interferometer<ref name=apj628_453/> and the Michigan InfraRed Combiner (MIRC)<ref name=spie62681P/> in the near infrared H band (see video below), allowing the orbital elements to be computed for the first time.<ref name=apj684_2_L95/>