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<rss version="2.0" xmlns:atom="http://www.w3.org/2005/Atom"><channel><title>A New Approach to Cosmological Bulk Viscosity · HackerPapers discussions</title><link>https://hackerpaper.kaipfister.de/p/1409.4918/</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/1409.4918/feed.xml" rel="self" type="application/rss+xml" /><item><title>A New Approach to Cosmological Bulk Viscosity — mentioned by raattgift</title><link>https://news.ycombinator.com/item?id=12192828</link><guid isPermaLink="false">urn:hackerpapers:mention:1409.4918:12192828</guid><pubDate>Sat, 30 Jul 2016 13:13:02 GMT</pubDate><description>&lt;p&gt;Nah, the second derivative of the scale factor in the second Friedmann equation (https://en.wikipedia.org/wiki/Friedmann_equations?oldformat=...) is still determined by energy-density (rho) and pressure (p). &amp;quot;p&amp;quot;, pressure, is equal to w \rho c^2, where w is a small negative number close to 0 (about -1/3 is a good fit for observation). Galaxies stars and atoms won&amp;#x27;t be ripped apart; instead you&amp;#x27;ll get these and structures mostly collapsing into supermassive black holes which occupy their own Hubble volumes (stray ejected stars and gas molecules will also eventually occupy their own Hubble…&lt;/p&gt;&lt;p&gt;&lt;a href="https://hackerpaper.kaipfister.de/p/1409.4918/"&gt;Paper and discussion history&lt;/a&gt;. A mention is not an endorsement.&lt;/p&gt;</description><category>gr-qc</category></item></channel></rss>
