GRB 230307A

230307A is the second brightest gamma ray burst detected in more than 50 years of observations and is located behind the Magellanic Bridge. Despite its long ...

A luminous precursor in the extremely bright GRB 230307A - arXiv

Title:A luminous precursor in the extremely bright GRB 230307A ... Abstract:GRB 230307A is an extremely bright long duration GRB with an observed ...

Heavy-element production in a compact object merger observed by ...

GRB 230307A is an extreme outlier of the >1,000 Swift GRBs, with an extremely faint afterglow for the brightness of its prompt emission. Other ...

NASA's Webb Makes First Detection of Heavy Element From Star ...

The case of GRB 230307A is particularly remarkable. First detected by Fermi in March, it is the second brightest GRB observed in over 50 ...

GRB 230307A - GCN - NASA

2010, 30L) located in South Africa (South African Astronomical Observatory) started inspect of the Fermi GRB 230307A ( Fermi GBM team, GCN 33405) errorbox 1 ...

[2402.10619] The Very Early Soft X-ray Plateau of GRB 230307A

This work explores that the Magnetar Wind Internal Gradual MAgnetic Dissipation (MIGMAD) model, in which the radiative efficiency evolves over time, ...

Further study of bright gamma-ray burst GRB 230307A shows it was ...

An international team of astronomers and astrophysicists has found evidence that the bright gamma-ray burst GRB 230307A observed last year ...

The Progenitor and Central Engine of a Peculiar GRB 230307A

The central engine of GRB 230307A is a magnetar that is originated from a binary compact star merger.

GRB 230307A: Fermi GBM Observation of a very bright burst

"At 15:44:06.67 UT on 07 March 2023, the Fermi Gamma-Ray Burst Monitor (GBM) triggered and located GRB 230307A (trigger 699896651 / 230307656).

possibly the second highest GRB energy fluence ever identified

Abstract. The very bright long GRB 230307A has been detected by many prompt GRB monitors (GCN Circ. 33405; Dalessi, GCN Circ. 33407; Dalessi and Roberts, ...

jet composition of GRB 230307A: Poynting-flux-dominated outflow?

The central engine of GRB 230307A is a millisecond magnetar which is the post-merger product of NS–NS mergers (supported by a lanthanide-rich kilonova). It can ...

A Luminous Precursor in the Extremely Bright GRB 230307A

Abstract. GRB 230307A is an extremely bright long-duration GRB with an observed gamma-ray fluence of ≳3 × 10−3 erg cm−2 (10–1000 keV), second ...

Evidence for a Compact Stellar Merger Origin for GRB 230307A ...

GRB 230307A is the second-brightest gamma-ray burst (GRB) ever detected over 50 yr of observations and has a long duration in the prompt ...

The environment of GRB 230307A. a, The false-color image...

The false-color image combines three filters from JWST (F 150W , F 277W , and F 444W ). The bright galaxy labeled by G1 is the most likely host galaxy at an ...

GRB 230307A Archives - the Astrobiology Web

“GRB 230307A”. Massive Space Explosion Observed Creating Elements Needed For Life · Astrochemistry · Massive Space Explosion Observed Creating Elements Needed ...

A Luminous Precursor in the Extremely Bright GRB 230307A

Abstract GRB 230307A is an extremely bright long-duration GRB with an observed gamma-ray fluence of ≳3 × 10 −3 erg cm −2 (10–1000 keV), second only to GRB ...

The Progenitor and Central Engine of a Peculiar GRB 230307A

Recently, a lack of supernova-associated with long-duration gamma-ray burst (GRB 230307A) at such a low redshift z = 0.065, but associated ...

Second-brightest gamma-ray burst ever seen observed creating ...

GRB 230307A lasted for 200 seconds, meaning it is categorized as a long-duration gamma-ray burst. This is unusual as short gamma-ray bursts, ...

A Luminous Precursor in the Extremely Bright GRB 230307A

Abstract. GRB 230307A is an extremely bright long-duration GRB with an observed gamma-ray fluence of ≳3 × 10−3 erg cm−2 (10-1000 keV), second ...

Evidence for a Compact Stellar Merger Origin for GRB 230307A ...

Abstract GRB 230307A is the second-brightest gamma-ray burst (GRB) ever detected over 50 yr of observations and has a long duration in the prompt emission.