2024MNRAS.530..555M

Query : 2024MNRAS.530..555M

2024MNRAS.530..555M - Mon. Not. R. Astron. Soc., 530, 555-559 (2024/May-1)

Constraints on the ultra-high energy cosmic ray output of gamma-ray bursts.

MOORE E., GENDRE B., ORANGE N.B. and PANTHER F.H.

Abstract (from CDS):

Ultra-high energy cosmic rays are the most extreme energetic particles detected on Earth, however, their acceleration sites are still mysterious. We explore the contribution of low-luminosity gamma-ray bursts to the ultra-high energy cosmic ray flux, since they form the bulk of the nearby population. We analyse a representative sample of these bursts detected by BeppoSAX, INTEGRAL, and Swift between 1998-2016, and found that in order to reconcile our theoretical flux with the observed flux, these bursts should accelerate at most 10–13 M⊙ of ultra-high energy cosmic rays.

Abstract Copyright: © 2024 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society.

Journal keyword(s): methods: statistical - gamma-ray burst: general - cosmic rays

Simbad objects: 44

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Number of rows : 44
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 101225A gB 00 00 47.48 +44 36 01.0           ~ 163 0
2 GRB 060912A gB 00 21 08.11 +20 58 18.9           ~ 116 1
3 Fermi bn120729456 gB 00 52 17.84 +49 56 23.1           ~ 122 0
4 GRB 151029A gB 02 34 06.71 -35 23 07.8           ~ 40 0
5 GRB 071112C gB 02 36 50.89 +28 22 16.9           ~ 164 0
6 GRB 140710A gB 02 44 16.26 +35 29 56.7           ~ 46 0
7 SN 2006aj SN* 03 21 39.670 +16 52 02.27 17.96 19.11 17.40     SNIc-BL 1007 1
8 GRB 151031A gB 05 32 47.02 -39 07 18.7           ~ 27 0
9 GRB 051117B gB 05 40 43.260 -19 16 26.10           ~ 77 0
10 GRB 050826 gB 05 51 01.590 -02 38 35.40           ~ 136 0
11 SN 2010bh SN* 07 10 30.63 -56 15 19.7           SNIc 336 1
12 GRB 051006 gB 07 23 13.520 +09 30 24.48           ~ 74 0
13 SN 2003lw SN* 08 02 30.1 -39 51 03       20.23   SNIc: 576 0
14 GRB 160117B gB 08 48 46.71 -16 22 00.9           ~ 41 0
15 Fermi bn110106893 gB 08 56 37.0 +47 00 10           ~ 82 0
16 SN 2012bz SN* 09 07 38.38 +14 01 07.5           SNIb/c 193 1
17 GRB 061021 gB 09 40 36.120 -21 57 05.40 18.21 19.20 16.82     ~ 160 0
18 SN 2013cq SN* 11 32 32.84 +27 41 56.2           SNIc 613 1
19 GRB 011121 gB 11 34 26.67 -76 01 41.6       23.0   ~ 286 1
20 GRB 070419A gB 12 10 58.830 +39 55 34.06 18.52         ~ 130 0
21 GRB 140318A gB 12 16 21.43 +20 12 32.5           ~ 41 0
22 GRB 130511A gB 13 06 34.89 +18 42 35.8           ~ 45 0
23 GRB 150727A gB 13 35 52.52 -18 19 32.7           ~ 59 0
24 GRB 050801 gB 13 36 35.000 -21 55 41.00 15.03 15.82 15.46     ~ 164 0
25 GRB 090417B gB 13 58 44.8 +47 00 55           ~ 119 1
26 SDSS J140910.47+275320.8 G 14 09 10.47535 +27 53 20.8393           ~ 279 0
27 GRB 120722A gB 15 21 58.0 +13 15 01           ~ 49 0
28 GRB 090814A gB 15 58 26.44 +25 37 52.4           ~ 56 0
29 GRB 100418A gB 17 05 26.96 +11 27 41.9           ~ 198 0
30 GRB 050223 gB 18 05 32.200 -62 28 20.40           ~ 109 0
31 GRB 050126 gB 18 32 27.22 +42 22 14.2           ~ 129 0
32 SN 2005nc SN* 18 32 32.560 +26 20 22.34           SNIc: 400 1
33 GRB 160425A gB 18 41 18.56 -54 21 36.1           ~ 49 0
34 SN 1998bw SN* 19 35 03.17 -52 50 46.1   14.09       SNIc 1928 2
35 Fermi bn161129300 gB 21 04 54.66 +32 08 05.5           ~ 65 0
36 GRB 060614 G 21 23 32.140 -53 01 36.10           ~ 714 0
37 GRB 060505 gB 22 07 03.440 -27 48 51.89           ~ 286 1
38 GRB 061110A gB 22 25 09.800 -02 15 30.70 21.43         ~ 134 0
39 SN 2008hw SN* 22 39 50.39 -40 08 49.1           SNIc 197 1
40 Fermi bn150821406 gB 22 47 39.15 -57 53 38.2           ~ 71 0
41 GRB 051109B gB 23 01 50.330 +38 40 46.51           ~ 93 0
42 GRB 201015A gB 23 37 16.43 +53 24 57.6           ~ 74 0
43 SN 2012eb SN* 23 41 38.35 -46 11 07.0           SNIb/c 62 1
44 SN 2013fu SN* 23 54 29.91 +29 25 47.6           SNIb/c 144 1

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