{"id":11,"date":"2021-12-15T15:26:49","date_gmt":"2021-12-15T14:26:49","guid":{"rendered":"https:\/\/home.phys.ntnu.no\/LOVE-NEST\/?page_id=11"},"modified":"2022-02-08T10:43:13","modified_gmt":"2022-02-08T09:43:13","slug":"science","status":"publish","type":"page","link":"https:\/\/home.phys.ntnu.no\/LOVE-NEST\/science\/","title":{"rendered":"Science"},"content":{"rendered":"<div class=\"wpb-content-wrapper\"><p>[vc_row css=&#8221;.vc_custom_1644313393369{background-color: rgba(255,255,255,0.8) !important;*background-color: rgb(255,255,255) !important;}&#8221;][vc_column][vc_column_text]<\/p>\n<h3>WHAT IS THE MAXIMUM MASS THAT A NEUTRON STAR CAN SUPPORT BEFORE COLLAPSING INTO A BLACK HOLE?<\/h3>\n<p>Theory tells us that this limit cannot be much higher than <strong>3<\/strong> Solar masses. Knowing the answer has a major impact on gravitational wave astronomy and nuclear physics.<\/p>\n<p>LOVE-NEST is focused on a new population of neutron stars in compact binaries known as \u201cspiders\u201d, because we have strong evidence that they harbor super-massive neutron stars.<\/p>\n<p>The <strong>first<\/strong> goal is to find many more &#8220;hidden spiders&#8221; by using multi-wavelength targeted searches.<\/p>\n<p>The <strong>second<\/strong> goal is to <strong>measure accurately their masses<\/strong>, using a new technique that we pioneered.<\/p>\n<p>The <strong>third<\/strong> goal is to model, simulate and <strong>understand the interaction between the relativistic pulsar wind and its surroundings<\/strong>. This will constrain the properties of the intrabinary shock between the pulsar and companion winds, which can accelerate particles up to at least 10s of TeVs.<\/p>\n<p>The impact of LOVE-NEST can reach further:<\/p>\n<ul>\n<li>the <strong>astroparticle physics<\/strong> community: the contribution of spiders to the cosmic rays and neutrinos observed on Earth remains largely unexplored.<\/li>\n<li>the <strong>nuclear physics<\/strong> community: the maximum neutron star mass depends on the microscopic interactions between particles in the core at densities of more than 10<sup>15<\/sup> g\/cm3.<\/li>\n<li>the rising field of <strong>gravitational wave astronomy<\/strong>: the signal and outcome of a double neutron star merger depends on the maximum mass of a neutron star.<\/li>\n<\/ul>\n<p>[\/vc_column_text][\/vc_column][\/vc_row]<\/p>\n<\/div>","protected":false},"excerpt":{"rendered":"<p>[vc_row css=&#8221;.vc_custom_1644313393369{background-color: rgba(255,255,255,0.8) !important;*background-color: rgb(255,255,255) !important;}&#8221;][vc_column][vc_column_text] WHAT IS THE MAXIMUM MASS THAT A NEUTRON STAR CAN SUPPORT BEFORE COLLAPSING INTO A BLACK HOLE? Theory tells us that this limit cannot be much higher than 3 Solar masses. Knowing the answer has a major impact on gravitational wave astronomy and nuclear physics. LOVE-NEST is focused on&hellip;<\/p>\n","protected":false},"author":1,"featured_media":0,"parent":0,"menu_order":0,"comment_status":"closed","ping_status":"closed","template":"","meta":{"footnotes":""},"class_list":["post-11","page","type-page","status-publish","hentry","description-off"],"_links":{"self":[{"href":"https:\/\/home.phys.ntnu.no\/LOVE-NEST\/wp-json\/wp\/v2\/pages\/11","targetHints":{"allow":["GET"]}}],"collection":[{"href":"https:\/\/home.phys.ntnu.no\/LOVE-NEST\/wp-json\/wp\/v2\/pages"}],"about":[{"href":"https:\/\/home.phys.ntnu.no\/LOVE-NEST\/wp-json\/wp\/v2\/types\/page"}],"author":[{"embeddable":true,"href":"https:\/\/home.phys.ntnu.no\/LOVE-NEST\/wp-json\/wp\/v2\/users\/1"}],"replies":[{"embeddable":true,"href":"https:\/\/home.phys.ntnu.no\/LOVE-NEST\/wp-json\/wp\/v2\/comments?post=11"}],"version-history":[{"count":0,"href":"https:\/\/home.phys.ntnu.no\/LOVE-NEST\/wp-json\/wp\/v2\/pages\/11\/revisions"}],"wp:attachment":[{"href":"https:\/\/home.phys.ntnu.no\/LOVE-NEST\/wp-json\/wp\/v2\/media?parent=11"}],"curies":[{"name":"wp","href":"https:\/\/api.w.org\/{rel}","templated":true}]}}