GW190425: Difference between revisions – Wikipedia

By /

From Wikipedia, the free encyclopedia

← Previous editNext edit →

Content deleted Content added


Line 1: Line 1:

{{Short description |Large binary neutron stars}}

{{Short description |Large binary neutron stars}}

{{Infobox astronomical object|name=GW190425|type=[[Binary neutron stars]]|onlysourced=[[LIGO]], [[Virgo interferometer]]|epoch=J2000|mass=3.4 [[Solar mass]]|luminosity_specify=159 light year|constellation=|ra=3. 12 <ref>https://cplberry.com/2020/01/06/gw190425/&sa=U&ved=2ahUKEwi4_vahzeqQAxVgZWwGHcX5MiA4ChAWegQIDRAC&usg=AOvVaw2aRdvelLlVJRDJidkx1S2M </ref>|dec=-0.17}}

{{Infobox astronomical object|name=GW190425|type=[[Binary neutron stars]]|onlysourced=[[LIGO]], [[Virgo interferometer]]|epoch=J2000|mass=3.4 [[Solar mass]]|luminosity_specify=159 light year|constellation=|ra=3. 12 <ref>https://cplberry.com/2020/01/06/gw190425/&sa=U&ved=2ahUKEwi4_vahzeqQAxVgZWwGHcX5MiA4ChAWegQIDRAC&usg=AOvVaw2aRdvelLlVJRDJidkx1S2M </ref>|dec=-0.17}}

”’GW190425”’ was a [[Gravitational wave|gravitational]] wave detected<ref>{{Cite journal |last1=Barbieri |first1=C. |last2=Salafia |first2=O. S. |last3=Colpi |first3=M. |last4=Ghirlanda |first4=G. |last5=Perego |first5=A. |date=2021-10-01 |title=Exploring the nature of ambiguous merging systems: GW190425 in low latency |url=https://www.aanda.org/articles/aa/abs/2021/10/aa37778-20/aa37778-20.html |journal=Astronomy & Astrophysics |language=en |volume=654 |pages=A12 |doi=10.1051/0004-6361/202037778 |bibcode=2021A&A…654A..12B |issn=0004-6361}}</ref><ref>{{Cite web |last=CPLB |date=2020-01-06 |title=GW190425—First discovery from O3 |url=https://cplberry.com/2020/01/06/gw190425/ |access-date=2025-11-11 |website=Christopher Berry |language=en}}</ref> on 19 April 2019 in LIGO<ref>{{Cite journal | last1=Abbott | first1=B. P. | last2=Abbott | first2=R. | last3=Abbott | first3=T. D. | last4=Abraham | first4=S. | last5=Acernese | first5=F. | last6=Ackley | first6=K. | last7=Adams | first7=C. | last8=Adhikari | first8=R. X. | last9=Adya | first9=V. B. | last10=Affeldt | first10=C. | last11=Agathos | first11=M. | last12=Agatsuma | first12=K. | last13=Aggarwal | first13=N. | last14=Aguiar | first14=O. D. | last15=Aiello | first15=L. | last16=Ain | first16=A. | last17=Ajith | first17=P. | last18=Allen | first18=G. | last19=Allocca | first19=A. | last20=Aloy | first20=M. A. | last21=Altin | first21=P. A. | last22=Amato | first22=A. | last23=Anand | first23=S. | last24=Ananyeva | first24=A. | last25=Anderson | first25=S. B. | last26=Anderson | first26=W. G. | last27=Angelova | first27=S. V. | last28=Antier | first28=S. | last29=Appert | first29=S. | last30=Arai | first30=K. | display-authors=1 |title=GW190425: Observation of a Compact Binary Coalescence with Total Mass ∼ 3.4 M<sub>⊙</sub> |journal=The Astrophysical Journal Letters | date=2020 | volume=892 | issue=1 | pages=L3 |doi=10.3847/2041-8213/ab75f5 | arxiv=2001.01761 | bibcode=2020ApJ…892L…3A | doi-access=free }}</ref> and [[Virgo interferometer|Virgo]]<ref>{{Cite journal |last1=Collaboration |first1=The LIGO Scientific |last2=Collaboration |first2=the Virgo |last3=Abbott |first3=B. P. |last4=Abbott |first4=R. |last5=Abbott |first5=T. D. |last6=Abraham |first6=S. |last7=Acernese |first7=F. |last8=Ackley |first8=K. |last9=Adams |first9=C. |date=2020-01-06 |title=GW190425: Observation of a Compact Binary Coalescence with Total Mass ∼ 3.4 M<sub>⊙</sub> |journal=The Astrophysical Journal Letters |volume=892 |pages=L3 |doi=10.3847/2041-8213/ab75f5 |doi-access=free |arxiv=2001.01761v3 |bibcode=2020ApJ…892L…3A |language=en}}</ref> interferometer. It was a compact binary coalescence<ref>{{Cite journal |last=Singh |first=Dr Kunal |date=2022-03-30 |title=High Frequency USG and Colour Doppler USG in Scrotal Swelling |journal=Journal of Medical Science and Clinical Research |volume=10 |issue=3 |doi=10.18535/jmscr/v10i3.25 |issn=2347-176X|doi-access=free }}</ref><ref>{{Cite journal |last1=Dudi |first1=Reetika |last2=Adhikari |first2=Ananya |last3=Brügmann |first3=Bernd |last4=Dietrich |first4=Tim |last5=Hayashi |first5=Kota |last6=Kawaguchi |first6=Kyohei |last7=Kiuchi |first7=Kenta |last8=Kyutoku |first8=Koutarou |last9=Shibata |first9=Masaru |last10=Tichy |first10=Wolfgang |date=2022-10-21 |title=Investigating GW190425 with numerical-relativity simulations |url=https://link.aps.org/doi/10.1103/PhysRevD.106.084039 |journal=Physical Review D |volume=106 |issue=8 |article-number=084039 |doi=10.1103/PhysRevD.106.084039 |arxiv=2109.04063 |bibcode=2022PhRvD.106h4039D }}</ref> with a signal to noise ratio 12.9. It is the result of a collision of two neutron stars or binary stars<ref>{{Cite web |title=GW190425: the merger of a compact binary with total mass of {{!}} ICCUB |url=https://icc.ub.edu/news/gw190425-merger-a-compact-binary-total-mass |access-date=2025-11-11 |website=icc.ub.edu}}</ref> with a total mass of 3.4 [[Solar mass|Solar]]<ref>{{Cite web |title=GW190425 |url = https://dcc.ligo.org/public/0161/P190425/007/gw190425-discovery.pdf&sa=U&ved=2ahUKEwjNnfHYy-qQAxXag2MGHU9qBmwQFnoECAkQAg&usg=AOvVaw0DxnTR5xavoyiTO-hitqfx}}</ref> masses<ref>{{Cite web |last=CPLB |date=2020-01-06 |title=GW190425—First discovery from O3 |url=https://cplberry.com/2020/01/06/gw190425/ |access-date=2025-11-11 |website=Christopher Berry |language=en}}</ref> (larger than any known [[Binary neutron stars|binary neutron]] stars).<ref>{{Cite web |title=INSPIRE |url=https://inspirehep.net/literature/2944599 |access-date=2025-11-11 |website=inspirehep.net}}</ref> Its host galaxy is likely [[UGC 10667]].<ref>{{Cite journal | last1=Magaña Hernandez | first1=Ignacio | last2=d’Emilio | first2=Virginia | last3=Morisaki | first3=Soichiro | last4=Bhardwaj | first4=Mohit | last5=Palmese | first5=Antonella |title=On the Association of GW190425 with Its Potential Electromagnetic Counterpart FRB 20190425A |journal=The Astrophysical Journal Letters | date=2024 | volume=971 | issue=1 | pages=L5 |doi=10.3847/2041-8213/ad5b4c | arxiv=2404.02496 | bibcode=2024ApJ…971L…5M | doi-access=free }}</ref>

”’GW190425”’ was a [[Gravitational wave|gravitational]] wave detected<ref>{{Cite journal |last1=Barbieri |first1=C. |last2=Salafia |first2=O. S. |last3=Colpi |first3=M. |last4=Ghirlanda |first4=G. |last5=Perego |first5=A. |date=2021-10-01 |title=Exploring the nature of ambiguous merging systems: GW190425 in low latency |url=https://www.aanda.org/articles/aa/abs/2021/10/aa37778-20/aa37778-20.html |journal=Astronomy & Astrophysics |language=en |volume=654 |pages=A12 |doi=10.1051/0004-6361/202037778 |bibcode=2021A&A…654A..12B |issn=0004-6361}}</ref><ref>{{Cite web |last=CPLB |date=2020-01-06 |title=GW190425—First discovery from O3 |url=https://cplberry.com/2020/01/06/gw190425/ |access-date=2025-11-11 |website=Christopher Berry |language=en}}</ref> on 19 April 2019 in LIGO<ref>{{Cite journal | last1=Abbott | first1=B. P. | last2=Abbott | first2=R. | last3=Abbott | first3=T. D. | last4=Abraham | first4=S. | last5=Acernese | first5=F. | last6=Ackley | first6=K. | last7=Adams | first7=C. | last8=Adhikari | first8=R. X. | last9=Adya | first9=V. B. | last10=Affeldt | first10=C. | last11=Agathos | first11=M. | last12=Agatsuma | first12=K. | last13=Aggarwal | first13=N. | last14=Aguiar | first14=O. D. | last15=Aiello | first15=L. | last16=Ain | first16=A. | last17=Ajith | first17=P. | last18=Allen | first18=G. | last19=Allocca | first19=A. | last20=Aloy | first20=M. A. | last21=Altin | first21=P. A. | last22=Amato | first22=A. | last23=Anand | first23=S. | last24=Ananyeva | first24=A. | last25=Anderson | first25=S. B. | last26=Anderson | first26=W. G. | last27=Angelova | first27=S. V. | last28=Antier | first28=S. | last29=Appert | first29=S. | last30=Arai | first30=K. | display-authors=1 |title=GW190425: Observation of a Compact Binary Coalescence with Total Mass ∼ 3.4 M<sub>⊙</sub> |journal=The Astrophysical Journal Letters | date=2020 | volume=892 | issue=1 | pages=L3 |doi=10.3847/2041-8213/ab75f5 | arxiv=2001.01761 | bibcode=2020ApJ…892L…3A | doi-access=free }}</ref> and [[Virgo interferometer|Virgo]]<ref>{{Cite journal |last1=Collaboration |first1=The LIGO Scientific |last2=Collaboration |first2=the Virgo |last3=Abbott |first3=B. P. |last4=Abbott |first4=R. |last5=Abbott |first5=T. D. |last6=Abraham |first6=S. |last7=Acernese |first7=F. |last8=Ackley |first8=K. |last9=Adams |first9=C. |date=2020-01-06 |title=GW190425: Observation of a Compact Binary Coalescence with Total Mass ∼ 3.4 M<sub>⊙</sub> |journal=The Astrophysical Journal Letters |volume=892 |pages=L3 |doi=10.3847/2041-8213/ab75f5 |doi-access=free |arxiv=2001.01761v3 |bibcode=2020ApJ…892L…3A |language=en}}</ref> interferometer. It was a compact binary coalescence<ref>{{Cite journal |last1=Dudi |first1=Reetika |last2=Adhikari |first2=Ananya |last3=Brügmann |first3=Bernd |last4=Dietrich |first4=Tim |last5=Hayashi |first5=Kota |last6=Kawaguchi |first6=Kyohei |last7=Kiuchi |first7=Kenta |last8=Kyutoku |first8=Koutarou |last9=Shibata |first9=Masaru |last10=Tichy |first10=Wolfgang |date=2022-10-21 |title=Investigating GW190425 with numerical-relativity simulations |url=https://link.aps.org/doi/10.1103/PhysRevD.106.084039 |journal=Physical Review D |volume=106 |issue=8 |article-number=084039 |doi=10.1103/PhysRevD.106.084039 |arxiv=2109.04063 |bibcode=2022PhRvD.106h4039D }}</ref> with a signal to noise ratio 12.9. It is the result of a collision of two neutron stars or binary stars<ref>{{Cite web |title=GW190425: the merger of a compact binary with total mass of {{!}} ICCUB |url=https://icc.ub.edu/news/gw190425-merger-a-compact-binary-total-mass |access-date=2025-11-11 |website=icc.ub.edu}}</ref> with a total mass of 3.4 [[Solar mass|Solar]]<ref>{{Cite web |title=GW190425 |url = https://dcc.ligo.org/public/0161/P190425/007/gw190425-discovery.pdf&sa=U&ved=2ahUKEwjNnfHYy-qQAxXag2MGHU9qBmwQFnoECAkQAg&usg=AOvVaw0DxnTR5xavoyiTO-hitqfx}}</ref> masses<ref>{{Cite web |last=CPLB |date=2020-01-06 |title=GW190425—First discovery from O3 |url=https://cplberry.com/2020/01/06/gw190425/ |access-date=2025-11-11 |website=Christopher Berry |language=en}}</ref> (larger than any known [[Binary neutron stars|binary neutron]] stars).<ref>{{Cite web |title=INSPIRE |url=https://inspirehep.net/literature/2944599 |access-date=2025-11-11 |website=inspirehep.net}}</ref> Its host galaxy is likely [[UGC 10667]].<ref>{{Cite journal | last1=Magaña Hernandez | first1=Ignacio | last2=d’Emilio | first2=Virginia | last3=Morisaki | first3=Soichiro | last4=Bhardwaj | first4=Mohit | last5=Palmese | first5=Antonella |title=On the Association of GW190425 with Its Potential Electromagnetic Counterpart FRB 20190425A |journal=The Astrophysical Journal Letters | date=2024 | volume=971 | issue=1 | pages=L5 |doi=10.3847/2041-8213/ad5b4c | arxiv=2404.02496 | bibcode=2024ApJ…971L…5M | doi-access=free }}</ref>

==References ==

==References ==

Revision as of 19:56, 12 December 2025

Large binary neutron stars

GW190425 was a gravitational wave detected[2][3] on 19 April 2019 in LIGO[4] and Virgo[5] interferometer. It was a compact binary coalescence[6] with a signal to noise ratio 12.9. It is the result of a collision of two neutron stars or binary stars[7] with a total mass of 3.4 Solar[8] masses[9] (larger than any known binary neutron stars).[10] Its host galaxy is likely UGC 10667.[11]

References

  1. ^ https://cplberry.com/2020/01/06/gw190425/&sa=U&ved=2ahUKEwi4_vahzeqQAxVgZWwGHcX5MiA4ChAWegQIDRAC&usg=AOvVaw2aRdvelLlVJRDJidkx1S2M [dead link]
  2. ^ Barbieri, C.; Salafia, O. S.; Colpi, M.; Ghirlanda, G.; Perego, A. (2021-10-01). “Exploring the nature of ambiguous merging systems: GW190425 in low latency”. Astronomy & Astrophysics. 654: A12. Bibcode:2021A&A…654A..12B. doi:10.1051/0004-6361/202037778. ISSN 0004-6361.
  3. ^ CPLB (2020-01-06). “GW190425—First discovery from O3”. Christopher Berry. Retrieved 2025-11-11.
  4. ^ Abbott, B. P.; et al. (2020). “GW190425: Observation of a Compact Binary Coalescence with Total Mass ∼ 3.4 M⊙“. The Astrophysical Journal Letters. 892 (1): L3. arXiv:2001.01761. Bibcode:2020ApJ…892L…3A. doi:10.3847/2041-8213/ab75f5.
  5. ^ Collaboration, The LIGO Scientific; Collaboration, the Virgo; Abbott, B. P.; Abbott, R.; Abbott, T. D.; Abraham, S.; Acernese, F.; Ackley, K.; Adams, C. (2020-01-06). “GW190425: Observation of a Compact Binary Coalescence with Total Mass ∼ 3.4 M⊙“. The Astrophysical Journal Letters. 892: L3. arXiv:2001.01761v3. Bibcode:2020ApJ…892L…3A. doi:10.3847/2041-8213/ab75f5.
  6. ^ Dudi, Reetika; Adhikari, Ananya; Brügmann, Bernd; Dietrich, Tim; Hayashi, Kota; Kawaguchi, Kyohei; Kiuchi, Kenta; Kyutoku, Koutarou; Shibata, Masaru; Tichy, Wolfgang (2022-10-21). “Investigating GW190425 with numerical-relativity simulations”. Physical Review D. 106 (8) 084039. arXiv:2109.04063. Bibcode:2022PhRvD.106h4039D. doi:10.1103/PhysRevD.106.084039.
  7. ^ “GW190425: the merger of a compact binary with total mass of | ICCUB”. icc.ub.edu. Retrieved 2025-11-11.
  8. ^ “GW190425”.
  9. ^ CPLB (2020-01-06). “GW190425—First discovery from O3”. Christopher Berry. Retrieved 2025-11-11.
  10. ^ “INSPIRE”. inspirehep.net. Retrieved 2025-11-11.
  11. ^ Magaña Hernandez, Ignacio; d’Emilio, Virginia; Morisaki, Soichiro; Bhardwaj, Mohit; Palmese, Antonella (2024). “On the Association of GW190425 with Its Potential Electromagnetic Counterpart FRB 20190425A”. The Astrophysical Journal Letters. 971 (1): L5. arXiv:2404.02496. Bibcode:2024ApJ…971L…5M. doi:10.3847/2041-8213/ad5b4c.

Must Read

Leave a Comment

Your email address will not be published. Required fields are marked *

Scroll to Top