Talk:R-process

message: This article seems OK to me. A few inter-wiki-links needed, what more?? Rursus 12:30, 23 January 2007 (UTC)
thread_title: Source citations needed?

message: In a project to update, expand, and contextualize the wikis relevant to stellar nucleosynthesis, I have made dramatic changes and added lots of information to the wiki.  Below I have retained a copy of the former version, so that you may feel free to compare the two.  The two major factual corrections I made: A=270 nuclei in the r-process are not the same as 'stable' A=270 elements on earth; they are far from stability, and it is hard to know without a citation what the Z value of these nuclei are.  Also, r-process abundance peaks are decidedly ~10 amu below s-process peaks, not above.  You can see this clearly on an N vs. Z diagram by finding the closed neutron shells near the neutron drip line and following them back on a constant A line to stability.  I have omitted to include the categories and other wiki tags for this paste for convenience.  DAID 07:51, 21 July 2007 (UTC)
thread_title: Large scale editing and re-write

message: The article has the phrase "first successful caricature of the r-process abundances".  Is 'caricature' really the right word for that?
Kashikom (talk) 03:29, 28 August 2014 (UTC)
thread_title:  Caricature or Characterization? 

message: A few images would make this article much more digestible. The intro section is quite verbose so maybe a large section of it could be incorporated into the main article. 
There is a large chunk of the nuclear physics section that goes into details specific to certain sites of the r-process. I think it would be good to put some of this in the "astrophysical sites" section but change it to a section about all sites of the r-process and subdivide it. Then the "nuclear physics" section can focus on considerations involved in the process itself such as reaction rates, waiting points, etc.
142.90.85.115 (talk) 22:24, 15 May 2018 (UTC)
thread_title:  Images/Intro/Excessive Supernovae Details? 

message: I suppose I understand the r-process, but I was wondering about the result of neutron star collisions.  If colliding neutron stars generate fragments small enough not to be neutron stars anymore, that is, the degeneracy pressure is large enough again, what do they decay into?  Where the r-process builds up larger nuclei, it seems to me that there should be a process that goes down from the high neutron density of neutron star fragments.  Or maybe I am imagining the liquid drop model too much.  Gah4 (talk) 06:30, 5 September 2018 (UTC)
replies: text: Can the article explain more about what happens when you decompress neutron star matter?  I understand the r-process as building up nuclei with incoming neutrons, but in the case of decompressing neutron star matter, it seems more like going down. Does it immediately separate into heavy nuclei sized pieces?  Slowly beta decay until enough protons have built up? Gah4 (talk) 00:35, 18 June 2019 (UTC)
thread_title:  neutron star parts 

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thread_title:  A Commons file used on this page has been nominated for deletion