Spin-down induced quark-hadron phase transition in cold isolated neutron stars

ABSTRACT We have studied the spin-down induced phase transition (PT) in cold, isolated neutron stars in this work. After birth, as the star slows down, its central density rises and crosses the critical density of PT, and a quark core is seeded inside the star. Intermediate-mass stars are more likel...

Ausführliche Beschreibung

Gespeichert in:
Bibliographische Detailangaben
Veröffentlicht in:Monthly notices of the Royal Astronomical Society 2022-09, Vol.516 (1), p.1127-1136
Hauptverfasser: Prasad, R, Mallick, Ritam
Format: Artikel
Sprache:eng
Online-Zugang:Volltext bestellen
Tags: Tag hinzufügen
Keine Tags, Fügen Sie den ersten Tag hinzu!
container_end_page 1136
container_issue 1
container_start_page 1127
container_title Monthly notices of the Royal Astronomical Society
container_volume 516
creator Prasad, R
Mallick, Ritam
description ABSTRACT We have studied the spin-down induced phase transition (PT) in cold, isolated neutron stars in this work. After birth, as the star slows down, its central density rises and crosses the critical density of PT, and a quark core is seeded inside the star. Intermediate-mass stars are more likely to have a quark seeding in their lifetime at birth. Smaller neutron stars do not have a quark core and remain neutron stars throughout their life, whereas in massive stars, a quark core exists at their centre from birth. In intermediate and massive stars, the quark core grows further as the star slows down. The appearance of a quark core leads to a sudden change in the moment of inertia of the star in its evolutionary history, and is also reflected in a sudden discontinuity in the braking index of the star (at the frequency where the quark core first seeds). The energy released during the PT process as the quark core is seeded can excite the f-mode oscillation in the star and is emitted in the form of the gravitational wave, which is in the range of detection with present operating detectors; however, future detectors will enable a more clean extraction of this signals. Also, neutrinos and bursts of gamma-rays can originate from PT events. The spin-down induced PT could be gradual or in the form of subsequent leaps producing persistent or multiple transient emissions.
doi_str_mv 10.1093/mnras/stac2324
format Article
fullrecord <record><control><sourceid>oup_TOX</sourceid><recordid>TN_cdi_crossref_primary_10_1093_mnras_stac2324</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><oup_id>10.1093/mnras/stac2324</oup_id><sourcerecordid>10.1093/mnras/stac2324</sourcerecordid><originalsourceid>FETCH-LOGICAL-c273t-54cd8433e24038776c4eb2bd971f4156029c7949395b775024a7e603942ed3593</originalsourceid><addsrcrecordid>eNqFkDtPwzAYRS0EEqGwMmdlcGv78yMeUcVLqmAA5sixHTWQ2sFOhPj3NBRmpruce690ELqkZEmJhtUuJJNXeTSWAeNHqKAgBWZaymNUEAICV4rSU3SW8xshhAOTBXp8HrqAXfwMZRfcZL0rPyaT3vHWuBRDOWxN9uWYTMjd2MWZKm3sXdnl2Jtxjwc_jTO5P075HJ20ps_-4jcX6PX25mV9jzdPdw_r6w22TMGIBbeu4gCecQKVUtJy37DGaUVbToUkTFuluQYtGqUEYdwoLwlozrwDoWGBloddm2LOybf1kLqdSV81JfVso_6xUf_Z2BeuDoU4Df-x361AYvk</addsrcrecordid><sourcetype>Aggregation Database</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype></control><display><type>article</type><title>Spin-down induced quark-hadron phase transition in cold isolated neutron stars</title><source>Oxford Journals Open Access Collection</source><creator>Prasad, R ; Mallick, Ritam</creator><creatorcontrib>Prasad, R ; Mallick, Ritam</creatorcontrib><description>ABSTRACT We have studied the spin-down induced phase transition (PT) in cold, isolated neutron stars in this work. After birth, as the star slows down, its central density rises and crosses the critical density of PT, and a quark core is seeded inside the star. Intermediate-mass stars are more likely to have a quark seeding in their lifetime at birth. Smaller neutron stars do not have a quark core and remain neutron stars throughout their life, whereas in massive stars, a quark core exists at their centre from birth. In intermediate and massive stars, the quark core grows further as the star slows down. The appearance of a quark core leads to a sudden change in the moment of inertia of the star in its evolutionary history, and is also reflected in a sudden discontinuity in the braking index of the star (at the frequency where the quark core first seeds). The energy released during the PT process as the quark core is seeded can excite the f-mode oscillation in the star and is emitted in the form of the gravitational wave, which is in the range of detection with present operating detectors; however, future detectors will enable a more clean extraction of this signals. Also, neutrinos and bursts of gamma-rays can originate from PT events. The spin-down induced PT could be gradual or in the form of subsequent leaps producing persistent or multiple transient emissions.</description><identifier>ISSN: 0035-8711</identifier><identifier>EISSN: 1365-2966</identifier><identifier>DOI: 10.1093/mnras/stac2324</identifier><language>eng</language><publisher>Oxford University Press</publisher><ispartof>Monthly notices of the Royal Astronomical Society, 2022-09, Vol.516 (1), p.1127-1136</ispartof><rights>2022 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society 2022</rights><lds50>peer_reviewed</lds50><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c273t-54cd8433e24038776c4eb2bd971f4156029c7949395b775024a7e603942ed3593</citedby><cites>FETCH-LOGICAL-c273t-54cd8433e24038776c4eb2bd971f4156029c7949395b775024a7e603942ed3593</cites><orcidid>0000-0003-2943-6388</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>314,780,784,1604,27924,27925</link.rule.ids><linktorsrc>$$Uhttps://dx.doi.org/10.1093/mnras/stac2324$$EView_record_in_Oxford_University_Press$$FView_record_in_$$GOxford_University_Press</linktorsrc></links><search><creatorcontrib>Prasad, R</creatorcontrib><creatorcontrib>Mallick, Ritam</creatorcontrib><title>Spin-down induced quark-hadron phase transition in cold isolated neutron stars</title><title>Monthly notices of the Royal Astronomical Society</title><description>ABSTRACT We have studied the spin-down induced phase transition (PT) in cold, isolated neutron stars in this work. After birth, as the star slows down, its central density rises and crosses the critical density of PT, and a quark core is seeded inside the star. Intermediate-mass stars are more likely to have a quark seeding in their lifetime at birth. Smaller neutron stars do not have a quark core and remain neutron stars throughout their life, whereas in massive stars, a quark core exists at their centre from birth. In intermediate and massive stars, the quark core grows further as the star slows down. The appearance of a quark core leads to a sudden change in the moment of inertia of the star in its evolutionary history, and is also reflected in a sudden discontinuity in the braking index of the star (at the frequency where the quark core first seeds). The energy released during the PT process as the quark core is seeded can excite the f-mode oscillation in the star and is emitted in the form of the gravitational wave, which is in the range of detection with present operating detectors; however, future detectors will enable a more clean extraction of this signals. Also, neutrinos and bursts of gamma-rays can originate from PT events. The spin-down induced PT could be gradual or in the form of subsequent leaps producing persistent or multiple transient emissions.</description><issn>0035-8711</issn><issn>1365-2966</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2022</creationdate><recordtype>article</recordtype><recordid>eNqFkDtPwzAYRS0EEqGwMmdlcGv78yMeUcVLqmAA5sixHTWQ2sFOhPj3NBRmpruce690ELqkZEmJhtUuJJNXeTSWAeNHqKAgBWZaymNUEAICV4rSU3SW8xshhAOTBXp8HrqAXfwMZRfcZL0rPyaT3vHWuBRDOWxN9uWYTMjd2MWZKm3sXdnl2Jtxjwc_jTO5P075HJ20ps_-4jcX6PX25mV9jzdPdw_r6w22TMGIBbeu4gCecQKVUtJy37DGaUVbToUkTFuluQYtGqUEYdwoLwlozrwDoWGBloddm2LOybf1kLqdSV81JfVso_6xUf_Z2BeuDoU4Df-x361AYvk</recordid><startdate>20220901</startdate><enddate>20220901</enddate><creator>Prasad, R</creator><creator>Mallick, Ritam</creator><general>Oxford University Press</general><scope>AAYXX</scope><scope>CITATION</scope><orcidid>https://orcid.org/0000-0003-2943-6388</orcidid></search><sort><creationdate>20220901</creationdate><title>Spin-down induced quark-hadron phase transition in cold isolated neutron stars</title><author>Prasad, R ; Mallick, Ritam</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c273t-54cd8433e24038776c4eb2bd971f4156029c7949395b775024a7e603942ed3593</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2022</creationdate><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Prasad, R</creatorcontrib><creatorcontrib>Mallick, Ritam</creatorcontrib><collection>CrossRef</collection><jtitle>Monthly notices of the Royal Astronomical Society</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext_linktorsrc</fulltext></delivery><addata><au>Prasad, R</au><au>Mallick, Ritam</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Spin-down induced quark-hadron phase transition in cold isolated neutron stars</atitle><jtitle>Monthly notices of the Royal Astronomical Society</jtitle><date>2022-09-01</date><risdate>2022</risdate><volume>516</volume><issue>1</issue><spage>1127</spage><epage>1136</epage><pages>1127-1136</pages><issn>0035-8711</issn><eissn>1365-2966</eissn><abstract>ABSTRACT We have studied the spin-down induced phase transition (PT) in cold, isolated neutron stars in this work. After birth, as the star slows down, its central density rises and crosses the critical density of PT, and a quark core is seeded inside the star. Intermediate-mass stars are more likely to have a quark seeding in their lifetime at birth. Smaller neutron stars do not have a quark core and remain neutron stars throughout their life, whereas in massive stars, a quark core exists at their centre from birth. In intermediate and massive stars, the quark core grows further as the star slows down. The appearance of a quark core leads to a sudden change in the moment of inertia of the star in its evolutionary history, and is also reflected in a sudden discontinuity in the braking index of the star (at the frequency where the quark core first seeds). The energy released during the PT process as the quark core is seeded can excite the f-mode oscillation in the star and is emitted in the form of the gravitational wave, which is in the range of detection with present operating detectors; however, future detectors will enable a more clean extraction of this signals. Also, neutrinos and bursts of gamma-rays can originate from PT events. The spin-down induced PT could be gradual or in the form of subsequent leaps producing persistent or multiple transient emissions.</abstract><pub>Oxford University Press</pub><doi>10.1093/mnras/stac2324</doi><tpages>10</tpages><orcidid>https://orcid.org/0000-0003-2943-6388</orcidid></addata></record>
fulltext fulltext_linktorsrc
identifier ISSN: 0035-8711
ispartof Monthly notices of the Royal Astronomical Society, 2022-09, Vol.516 (1), p.1127-1136
issn 0035-8711
1365-2966
language eng
recordid cdi_crossref_primary_10_1093_mnras_stac2324
source Oxford Journals Open Access Collection
title Spin-down induced quark-hadron phase transition in cold isolated neutron stars
url https://sfx.bib-bvb.de/sfx_tum?ctx_ver=Z39.88-2004&ctx_enc=info:ofi/enc:UTF-8&ctx_tim=2024-12-21T17%3A40%3A18IST&url_ver=Z39.88-2004&url_ctx_fmt=infofi/fmt:kev:mtx:ctx&rfr_id=info:sid/primo.exlibrisgroup.com:primo3-Article-oup_TOX&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.genre=article&rft.atitle=Spin-down%20induced%20quark-hadron%20phase%20transition%20in%20cold%20isolated%20neutron%20stars&rft.jtitle=Monthly%20notices%20of%20the%20Royal%20Astronomical%20Society&rft.au=Prasad,%20R&rft.date=2022-09-01&rft.volume=516&rft.issue=1&rft.spage=1127&rft.epage=1136&rft.pages=1127-1136&rft.issn=0035-8711&rft.eissn=1365-2966&rft_id=info:doi/10.1093/mnras/stac2324&rft_dat=%3Coup_TOX%3E10.1093/mnras/stac2324%3C/oup_TOX%3E%3Curl%3E%3C/url%3E&disable_directlink=true&sfx.directlink=off&sfx.report_link=0&rft_id=info:oai/&rft_id=info:pmid/&rft_oup_id=10.1093/mnras/stac2324&rfr_iscdi=true