2024ApJ...976L..20S

Query : 2024ApJ...976L..20S

2024ApJ...976L..20S - Astrophys. J., 976, L20 (2024/December-1)

GRB 240529A: A Tale of Two Shocks.

SUN T.-R., GENG J.-J., YAN J.-Z., HU Y.-D., WU X.-F., CASTRO-TIRADO A.J., YANG C., PING Y.-D., HU C.-R., XU F., GAO H.-X., JIANG J.-A., ZHU Y.-T., XUE Y., PEREZ-GARCIA I., WU S.-Y., FERNANDEZ-GARCIA E., CABALLERO-GARCIA M.D., SANCHEZ-RAMIREZ R., GUZIY S., OLIVARES I., PEREZ DEL PULGAR C.J., CASTELLON A., CASTILLO S., XIONG D.-R., PANDEY S.B., HIRIART D., GARCIA-SEGURA G., LEE W.H., CARRASCO-GARCIA I.M., PARK I.H., JEONG S., MEINTJES P.J., VAN HEERDEN H.J., MARTIN-CARRILLO A., HANLON L., ZHANG B.-B., HERNANDEZ-GARCIA L., GRITSEVICH M., ROSSI A., MAIORANO E., CUSANO F., D'AVANZO P., FERRO M., MELANDRI A., DE PASQUALE M., BRIVIO R., FANG M., FAN L.-L., HU W.-D., WAN Z., HU L., ZUO Y.-X., TANG J.-L., ZHANG X.-L., ZHENG X.-Z., LI B., LUO W.-T., LIU W., WANG J., ZHANG H.-F., LIU H., GAO J., LIANG M., WANG H.-R., YAO D.-Z., CHENG J.-Q., ZHAO W. and DAI Z.-G.

Abstract (from CDS):

Thanks to the rapidly increasing time-domain facilities, we are entering a golden era of research on gamma-ray bursts (GRBs). In this Letter, we report our observations of GRB 240529A with the Burst Optical Observer and Transient Exploring System, the 1.5 m telescope at Observatorio de Sierra Nevada, the 2.5 m Wide Field Survey Telescope of China, the Large Binocular Telescope, and the Telescopio Nazionale Galileo. The prompt emission of GRB 240529A shows two comparable energetic episodes separated by a quiescence time of roughly 400 s. Combining all available data on the GRB Coordinates Network, we reveal the simultaneous apparent X-ray plateau and optical rebrightening around 103-104 s after the burst. Rather than the energy injection from the magnetar as widely invoked for similar GRBs, the multiwavelength emissions could be better explained as two shocks launched from the central engine separately. The optical peak time and our numerical modeling suggest that the initial bulk Lorentz factor of the later shock is roughly 50, which indicates that the later jet should be accretion driven and have a higher mass loading than a typical one. The quiescence time between the two prompt emission episodes may be caused by the transition between different accretion states of a central magnetar or black hole, or the fallback accretion process. A sample of similar bursts with multiple emission episodes in the prompt phase and sufficient follow-up could help to probe the underlying physics of GRB central engines.

Abstract Copyright: © 2024. The Author(s). Published by the American Astronomical Society.

Journal keyword(s): Gamma-ray bursts - High energy astrophysics - Non-thermal radiation sources - Optical observation - Relativistic jets

Status at CDS : Large table(s) will be appraised for possible ingestion in VizieR.

Simbad objects: 1

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Number of rows : 1
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 GRB 240529A gB 22 21 22 +51 33.4           ~ 9 0

Query : 2024ApJ...976L..20S

Basic data :
GRB 240529A -- Gamma-ray Burst
Other object types: otypes_help 		gB (GRB)
ICRS coord. (ep=J2000) : 		22 21 21.8 +51 33 25 (Gamma-ray) [ ] E 2024ApJ...976L..20S
FK4 coord. (ep=B1950 eq=1950) : 		22 19 23.3 +51 18 16 [ ]
Gal coord. (ep=J2000) : 		100.6032 -04.6889 [ ]
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Identifiers (1) :
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GRB 240529A

References (9 between 1850 and 2026) (Total 9)
Simbad bibliographic survey began in 1850 for stars (at least bright stars) and in 1983 for all other objects (outside the solar system).
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