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<rss version="2.0" xmlns:atom="http://www.w3.org/2005/Atom"><channel><title>Circumbinary Accretion: From Binary Stars to Massive Binary Black Holes · HackerPapers discussions</title><link>https://hackerpaper.kaipfister.de/p/2211.00028/</link><description>Collected HN comments and submissions linking this paper.</description><language>en</language><lastBuildDate>Mon, 02 Nov 2026 11:16:22 GMT</lastBuildDate><atom:link href="https://hackerpaper.kaipfister.de/p/2211.00028/feed.xml" rel="self" type="application/rss+xml" /><item><title>Circumbinary Accretion: From Binary Stars to Massive Binary Black Holes — mentioned by raattgift</title><link>https://news.ycombinator.com/item?id=39971410</link><guid isPermaLink="false">urn:hackerpapers:mention:2211.00028:39971410</guid><pubDate>Mon, 08 Apr 2024 16:37:22 GMT</pubDate><description>&lt;p&gt;&amp;gt; If you (the neutron star) gain mass near the gravitational field, it pulls you in closer. This conflicts with the Strong Equivalence Principle (SEP) in its universality of free fall form, or more colloquially a rule that the trajectory of a self-gravitating object depends only on its initial position and velocity and not on its internal composition (including the evolution of its mass). There is a good test of the SEP in a system involving the millisecond pulsar https://en.wikipedia.org/wiki/PSR_J0337%2B1715 which is in a hard binary with a white dwarf; a second white dwarf orbits the inner…&lt;/p&gt;&lt;p&gt;&lt;a href="https://hackerpaper.kaipfister.de/p/2211.00028/"&gt;Paper and discussion history&lt;/a&gt;. A mention is not an endorsement.&lt;/p&gt;</description><category>astro-ph.HE</category></item></channel></rss>
