<?xml version="1.0" encoding="UTF-8"?>
<rss version="2.0" xmlns:atom="http://www.w3.org/2005/Atom"><channel><title>Millisecond Pulsars as Tools of Fundamental Physics · HackerPapers discussions</title><link>https://hackerpaper.kaipfister.de/p/astro-ph_0405178/</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/astro-ph_0405178/feed.xml" rel="self" type="application/rss+xml" /><item><title>Millisecond Pulsars as Tools of Fundamental Physics — mentioned by raattgift</title><link>https://news.ycombinator.com/item?id=16297767</link><guid isPermaLink="false">urn:hackerpapers:mention:astro-ph_0405178:16297767</guid><pubDate>Sat, 03 Feb 2018 14:39:18 GMT</pubDate><description>&lt;p&gt;Er, can you characterize which post-Newtonian correction/s is or are of non-negligible order here for Milky-way millisecond pulsars? Where do they enter, if not extremely close to the pulsars themselves? I&amp;#x27;m curious, because we use them to test, among other things, |\alpha_3| in the PPN formalism alpha-zeta notation. Along the way you necessarily get a very good characterization of the transforms available on local arrival times in different coordinate systems and can probe other PPN parameters. (cf. Kramer, sec 4 and 5.1 free version: http://arxiv.org/abs/astro-ph/0405178v2). More generally…&lt;/p&gt;&lt;p&gt;&lt;a href="https://hackerpaper.kaipfister.de/p/astro-ph_0405178/"&gt;Paper and discussion history&lt;/a&gt;. A mention is not an endorsement.&lt;/p&gt;</description><category>astro-ph</category></item></channel></rss>
