2014MNRAS.438.3243R


C.D.S. - SIMBAD4 rel 1.7 - 2021.04.14CEST13:53:39

2014MNRAS.438.3243R - Mon. Not. R. Astron. Soc., 438, 3243-3254 (2014/March-2)

X-ray decay lines from heavy nuclei in supernova remnants as a probe of the r-process origin and the birth periods of magnetars.

RIPLEY J.L., METZGER B.D., ARCONES A. and MARTINEZ-PINEDO G.

Abstract (from CDS):

The origin of rapid neutron capture (r-process) nuclei remains one of the longest standing mysteries in nuclear astrophysics. Core collapse supernovae (SNe) and neutron star binary mergers are likely r-process sites, but little evidence yet exists for their in situ formation in such environments. Motivated by the advent of sensitive new or planned X-ray telescopes such as the Nuclear Spectroscopic Telescope Array (NuSTAR) and the Large Observatory for X-ray Timing (LOFT), we revisit the prospects for the detection of X-ray decay lines from r-process nuclei in young or nearby supernova remnants. For all remnants planned to be observed by NuSTAR (and several others), we conclude that r-process nuclei are detectable only if the remnant possesses a large overabundance O \gtrsim 10^3 relative to the average yield per SN. Prospects are better for the next Galactic SN (assumed age of 3yr and distance of 10 kpc), for which an average r-process yield is detectable via the 10.7 (9.2) keV line complexes of 194Os by LOFT at 6σ (5σ) confidence; the 27.3keV line complex of 125Sb is detectable by NuSTAR at 2σ for O \gtrsim 2. We also consider X-rays lines from the remnants of Galactic magnetars, motivated by the much higher r-process yields of the magnetorotationally driven SNe predicted to birth magnetars. The ∼ 3.6-3.9keV lines of 126Sn are potentially detectable in the remnants of the magnetars 1E1547.0-5408 and 1E2259+586 by LOFT for an assumed r-process yield predicted by recent simulations. The (non-)detection of these lines can thus probe whether magnetars are indeed born with millisecond periods. Finally, we consider a blind survey of the Galactic plane with LOFT for r-process lines from the most recent binary neutron star merger remnant, concluding that a detection is unlikely without additional information on the merger location.

Abstract Copyright: © 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society (2014)

Journal keyword(s): line: formation - nuclear reactions, nucleosynthesis, abundances - stars: abundances - stars: magnetars - stars: neutron - X-rays: general

Simbad objects: 13

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Number of rows : 13

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 PSR J0146+6145 Psr 01 46 22.21 +61 45 03.8   28.100 25.620     ~ 518 0
2 2XMM J050106.5+451634 X 05 01 08.0 +45 16 31           ~ 110 0
3 PSR B0525-66 Psr 05 26 00.7 -66 04 35           ~ 524 1
4 SN 1987A SN* 05 35 28.020 -69 16 11.07           SNIIpec 4577 2
5 NAME Vela Jr SN SNR 08 52.0 -46 20           ~ 421 2
6 NAME Lupus SN SNR 15 02 22.1 -42 05 49           ~ 1231 1
7 PSR J1550-5418 Psr 15 50 54.18 -54 18 23.9           ~ 352 1
8 [AAB2008] 1 X 17 14 05.758 -38 10 31.32           ~ 51 1
9 SNR G001.9+00.3 SNR 17 48 46.10 -27 09 50.9           ~ 172 1
10 PSR J1841-0456 Psr 18 41 19.29 -04 56 11.4           ~ 239 1
11 AX J1844.8-0258 HXB 18 44 53 -02 56.0           ~ 112 0
12 2E 4673 HXB 23 01 08.14 +58 52 44.5           ~ 597 1
13 NAME Cas A SNR 23 23 24.000 +58 48 54.00     14.30     ~ 2487 1

    Equat.    Gal    SGal    Ecl

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