2023ApJ...957...55Z

Query : 2023ApJ...957...55Z

2023ApJ...957...55Z - Astrophys. J., 957, 55 (2023/November-1)

Magnetic Structures and Turbulence in SN 1006 Revealed with Imaging X-Ray Polarimetry.

ZHOU P., PROKHOROV D., FERRAZZOLI R., YANG Y.-J., SLANE P., VINK J., SILVESTRI S., BUCCIANTINI N., REYNOSO E., MOFFETT D., SOFFITTA P., SWARTZ D., KAARET P., BALDINI L., COSTA E., NG C.-Y., KIM D.E., DOROSHENKO V., EHLERT S.R., HEYL J., MARIN F., MIZUNO T., PESCE-ROLLINS M., SGRO C., TAMAGAWA T., WEISSKOPF M.C., XIE F., AGUDO I., ANTONELLI L.A., BACHETTI M., BAUMGARTNER W.H., BELLAZZINI R., BIANCHI S., BONGIORNO S.D., BONINO R., BREZ A., CAPITANIO F., CASTELLANO S., CAVAZZUTI E., CHEN C.-T., CIPRINI S., DE ROSA A., DEL MONTE E., DI GESU L., DI LALLA N., DI MARCO A., DONNARUMMA I., DOVCIAK M., ENOTO T., EVANGELISTA Y., FABIANI S., GARCIA J.A., GUNJI S., HAYASHIDA K., IWAKIRI W., JORSTAD S.G., KISLAT F., KARAS V., KITAGUCHI T., KOLODZIEJCZAK J.J., KRAWCZYNSKI H., LA MONACA F., LATRONICO L., LIODAKIS I., MALDERA S., MANFREDA A., MARINUCCI A., MARSCHER A.P., MARSHALL H.L., MATT G., MITSUISHI I., MULERI F., NEGRO M., O'DELL S.L., OMODEI N., OPPEDISANO C., PAPITTO A., PAVLOV G.G., PEIRSON A.L., PERRI M., PETRUCCI P.-O., PILIA M., POSSENTI A., POUTANEN J., PUCCETTI S., RAMSEY B.D., RANKIN J., RATHEESH A., ROBERTS O., ROMANI R.W., SPANDRE G., TAVECCHIO F., TAVERNA R., TAWARA Y., TENNANT A.F., THOMAS N.E., TOMBESI F., TROIS A., TSYGANKOV S.S., TUROLLA R., WU K. and ZANE S.

Abstract (from CDS):

Young supernova remnants strongly modify the surrounding magnetic fields, which in turn play an essential role in accelerating cosmic rays (CRs). The X-ray polarization measurements probe magnetic field morphology and turbulence at the immediate acceleration site. We report the X-ray polarization distribution in the northeastern shell of SN 1006 from a 1 Ms observation with the Imaging X-ray Polarimetry Explorer. We found an average polarization degree of 22.4% ± 3.5% and an average polarization angle of -45.°4 ± 4.°5 (measured on the plane of the sky from north to east). The X-ray polarization angle distribution reveals that the magnetic fields immediately behind the shock in the northeastern shell of SN 1006 are nearly parallel to the shock normal or radially distributed, similar to that in the radio observations, and consistent with the quasi-parallel CR acceleration scenario. The X-ray emission is marginally more polarized than that in the radio band. The X-ray polarization degree of SN 1006 is much larger than that in Cas A and Tycho, together with the relatively tenuous and smooth ambient medium of the remnant, favoring that CR-induced instabilities set the magnetic turbulence in SN 1006, and CR acceleration is environment-dependent.

Abstract Copyright: © 2023. The Author(s). Published by the American Astronomical Society.

Journal keyword(s): Supernova remnants - Polarimetry - X-ray astronomy - Shocks - Cosmic rays

Simbad objects: 3

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Number of rows : 3
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 SN 1572A SN* 00 25 21.5 +64 08 27           B8 1254 1
2 NAME Lupus SN SNR 15 02 22.1 -42 05 49           ~ 1407 1
3 NAME Cas A SNR 23 23 26.0 +58 48 41     14.30     ~ 3033 1

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