Navegar

Colección

Datos Estadísticas

Artículo

Estamos trabajando para incorporar este artículo al repositorio
Consulte el artículo en la página del editor
Consulte la política de Acceso Abierto del editor

Abstract:

Radio polarization observations provide essential information on the degree of order and orientation of magnetic fields, which themselves play a key role in the particle acceleration processes that take place in supernova remnants (SNRs). Here we present a radio polarization study of SN 1006, based on combined Very Large Array and Australia Telescope Compact Array observations at 20 cm that resulted in sensitive images with an angular resolution of 10 arcsec. The fractional polarization in the two bright radio and X-ray lobes of the SNR is measured to be 0.17, while in the southeastern sector, where the radio and non-thermal X-ray emission are much weaker, the polarization fraction reaches a value of 0.6 ± 0.2, close to the theoretical limit of 0.7. We interpret this result as evidence of a disordered, turbulent magnetic field in the lobes, where particle acceleration is believed to be efficient, and a highly ordered field in the southeast, where the acceleration efficiency has been shown to be very low. Utilizing the frequency coverage of our observations, an average rotation measure of ∼12 rad m-2 is determined from the combined data set, which is then used to obtain the intrinsic direction of the magnetic field vectors. While the orientation of magnetic field vectors across the SNR shell appear to be radial, a large fraction of the magnetic vectors lie parallel to the Galactic plane. Along the highly polarized southeastern rim, the field is aligned tangent to the shock, and therefore also nearly parallel to the Galactic plane. These results strongly suggest that the ambient field surrounding SN 1006 is aligned with this direction (i.e., from northeast to southwest) and that the bright lobes are due to a polar cap geometry. Our study establishes that the most efficient particle acceleration and generation of magnetic turbulence in SN 1006 is attained for shocks in which the magnetic field direction and shock normal are quasi-parallel, while inefficient acceleration and little to no generation of magnetic turbulence are obtained for the quasi-perpendicular case. © 2013. The American Astronomical Society. All rights reserved.

Registro:

Documento: Artículo
Título:On the radio polarization signature of efficient and inefficient particle acceleration in supernova remnant SN 1006
Autor:Reynoso, E.M.; Hughes, J.P.; Moffett, D.A.
Filiación:Instituto de Astronomía y Física Del Espacio (IAFE), C. C. 67, Suc. 28, 1428 Buenos Aires, Argentina
Department of Physics and Astronomy, Rutgers University, Piscataway, NJ 08854-8019, United States
Department of Physics, Furman University, Greenville, SC 29613, United States
FCEyN, UBA, Argentina
Palabras clave:acceleration of particles; ISM: individual objects (SN 1006); ISM: supernova remnants; magnetic fields; polarization
Año:2013
Volumen:145
Número:4
DOI: http://dx.doi.org/10.1088/0004-6256/145/4/104
Título revista:Astronomical Journal
Título revista abreviado:Astron. J.
ISSN:00046256
Registro:https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046256_v145_n4_p_Reynoso

Referencias:

  • Acero, F., Aharonian, F., Akhperjanian, A.G., (2010) A&A, 516, p. 62. , 10.1051/0004-6361/200913916 0004-6361
  • Acero, F., Ballet, J., Decourchelle, A., The gas density around SN 1006 (2007) Astronomy and Astrophysics, 475 (3), pp. 883-890. , DOI 10.1051/0004-6361:20077742
  • Axford, W.I., Leer, E., Skadron, G., (1977) Proc. 15th Int. Cosmic Ray Conf., 11, p. 132
  • Bell, A.R., (1978) MNRAS, 182, p. 147. , 0035-8711
  • Bell, A.R., (1978) MNRAS, 182, p. 443. , 0035-8711
  • Bell, A.R., Turbulent amplification of magnetic field and diffusive shock acceleration of cosmic rays (2004) Monthly Notices of the Royal Astronomical Society, 353 (2), pp. 550-558. , DOI 10.1111/j.1365-2966.2004.08097.x
  • Bell, A.R., Lucek, S.G., Cosmic ray acceleration to very high energy through the non-linear amplification by cosmic rays of the seed magnetic field (2001) Monthly Notices of the Royal Astronomical Society, 321 (3), pp. 433-438. , DOI 10.1046/j.1365-8711.2001.04063.x
  • Blandford, R.D., Ostriker, J.P., (1978) ApJL, 221, p. 29. , 10.1086/182658 0004-637X
  • Burn, B.J., (1966) MNRAS, 133, p. 67. , 0035-8711
  • Cassam-Chenaï, G., Hughes, J.P., Reynoso, E.M., Badenes, C., Moffett, D., (2008) ApJ, 680 (2), p. 1180. , 10.1086/588015 0004-637X 1180
  • Decourchelle, A., Ellison, D.C., Ballet, J., (2000) ApJL, 543, p. 57. , 10.1086/318167 0004-637X
  • Dickel, J.R., Milne, D.K., (1976) AuJPh, 29, p. 435
  • Dickel, J.R., Milne, D.K., Strom, R.G., (2000) ApJ, 543 (2), p. 840. , 10.1086/317160 0004-637X 840
  • Dolginov, A.Z., Podol'Skaya, N.I., Toptygin, I.N., (2004) AstL, 30, p. 169
  • Dyer, K.K., Cornwell, T.J., Maddalena, R.J., (2009) AJ, 137 (2), p. 2956. , 10.1088/0004-6256/137/2/2956 1538-3881 2956
  • Dyer, K.K., Reynolds, S.P., Borkowski, K.J., (2004) ApJ, 600 (2), p. 752. , 10.1086/380093 0004-637X 752
  • Ellison, D.C., Baring, M.G., Jones, F.C., (1995) ApJ, 453, p. 873. , 10.1086/176447
  • Fulbright, M.S., Reynolds, S.P., (1990) ApJ, 357, p. 591. , 10.1086/168947
  • Ghavamian, P., Frank Winkler, P., Raymond, J.C., Long, K.S., The optical spectrum of the SN 1006 supernova remnant revisited (2002) Astrophysical Journal, 572 (2), pp. 888-896. , DOI 10.1086/340437
  • Gotthelf, E.V., Koralesky, B., Rudnick, L., (2001) ApJL, 552, p. 39. , 10.1086/320250 0004-637X
  • Harvey-Smith, L., Gaensler, B.M., Kothes, R., (2010) ApJ, 712 (2), p. 1157. , 10.1088/0004-637X/712/2/1157 0004-637X 1157
  • Jokipii, J.R., (1987) ApJ, 313, p. 842. , 10.1086/165022
  • Jun, B.-I., Norman, M.L., On the Origin of Radial Magnetic Fields in Young Supernova Remnants (1996) Astrophysical Journal, 472 (1 NUMBER 1), pp. 245-256. , DOI 10.1086/178059
  • Krymskii, G.F., (1977) DoSSR, 234, p. 1306
  • Kundu, M.R., (1970) ApJ, 162, p. 17. , 10.1086/150630
  • Landecker, T.L., Routledge, D., Reynolds, S.P., (1999) ApJ, 527 (2), p. 866. , 10.1086/308100 0004-637X 866
  • Lauberts, A., (1982) The ESO/Uppsala Survey of the ESO(B) Atlas
  • Malkov, M.A., O'C Drury, L., (2001) RPPh, 64, p. 429
  • Milne, D.K., (1971) AuJPh, 24, p. 757
  • Milne, D.K., (1987) AuJPh, 40, p. 771
  • Petruk, O., Beshley, V., Bocchino, F., Miceli, M., Orlando, S., (2011) MNRAS, 413, p. 1643. , 10.1111/j.1365-2966.2011.18237.x 0035-8711
  • Petruk, O., Dubner, G., Castelletti, G., (2009) MNRAS, 393, p. 1034. , 10.1111/j.1365-2966.2008.14251.x 0035-8711
  • Petruk, O., Kuzyo, T., Bocchino, F., (2012) MNRAS, 419, p. 608. , 10.1111/j.1365-2966.2011.19722.x 0035-8711
  • Reynolds, S.P., Gilmore, D.M., (1986) AJ, 92, p. 1138. , 10.1086/114244 1548-9558
  • Reynolds, S.P., Gilmore, D.M., (1993) AJ, 106, p. 272. , 10.1086/116635
  • Reynoso, E.M., Green, A.J., (2007) MNRAS, 375, p. 92. , 10.1111/j.1365-2966.2006.11264.x 0035-8711
  • Reynoso, E.M., Moffett, D.A., Goss, W.M., Dubner, G.M., Dickel, J.R., Reynolds, S.P., Giacani, E.B., A VLA Study of the Expansion of Tycho's Supernova Remnant (1997) Astrophysical Journal, 491 (2 NUMBER 1), pp. 816-828. , DOI 10.1086/304997
  • Rothenflug, R., Ballet, J., Dubner, G., (2004) A&A, 425, p. 121. , 10.1051/0004-6361:20047104 0004-6361
  • Saikia, D.J., (1999) MNRAS, 302, p. 60. , 10.1046/j.1365-8711.1999.02295.x 0035-8711
  • Sault, R.J., Teuben, P.J., Wright, M.C.H., (1995) Astronomical Data Analysis Software and Systems IV, p. 433
  • Schneiter, E.M., Velázquez, P.F., Reynoso, E.M., De Colle, F., (2010) MNRAS, 408, p. 430. , 10.1111/j.1365-2966.2010.17125.x 0035-8711
  • Stephenson, F.R., Green, D.A., (2002) Historical Supernovae and Their Remnants, , 10.1093/acprof:oso/9780198507666.001.0001
  • Warren, J.S., Hughes, J.P., Badenes, C., Ghavamian, P., Mckee, C.F., Moffett, D., Plucinsky, P.P., Slane, P., Cosmic-ray acceleration at the forward shock in Tycho's supernova remnant: Evidence from Chandra X-ray observations (2005) Astrophysical Journal, 634 (1), pp. 376-389. , DOI 10.1086/496941
  • Winkler, P.F., Gupta, G., Long, K.S., The SN 1006 remnant: Optical proper motions, deep imaging, distance, and brightness at maximum (2003) Astrophysical Journal, 585 (1), pp. 324-335. , DOI 10.1086/345985
  • Frank Winkler, P., Long, K.S., X-Ray and Optical Imagery of the SN 1006 Supernova Remnant (1997) Astrophysical Journal, 491 (2 NUMBER 1), pp. 829-838. , DOI 10.1086/304969
  • Wood, C.A., Mufson, S.L., Dickel, J.R., (2008) AJ, 135 (6), p. 2358. , 10.1088/0004-6256/135/6/2358 1538-3881 2358

Citas:

---------- APA ----------
Reynoso, E.M., Hughes, J.P. & Moffett, D.A. (2013) . On the radio polarization signature of efficient and inefficient particle acceleration in supernova remnant SN 1006. Astronomical Journal, 145(4).
http://dx.doi.org/10.1088/0004-6256/145/4/104
---------- CHICAGO ----------
Reynoso, E.M., Hughes, J.P., Moffett, D.A. "On the radio polarization signature of efficient and inefficient particle acceleration in supernova remnant SN 1006" . Astronomical Journal 145, no. 4 (2013).
http://dx.doi.org/10.1088/0004-6256/145/4/104
---------- MLA ----------
Reynoso, E.M., Hughes, J.P., Moffett, D.A. "On the radio polarization signature of efficient and inefficient particle acceleration in supernova remnant SN 1006" . Astronomical Journal, vol. 145, no. 4, 2013.
http://dx.doi.org/10.1088/0004-6256/145/4/104
---------- VANCOUVER ----------
Reynoso, E.M., Hughes, J.P., Moffett, D.A. On the radio polarization signature of efficient and inefficient particle acceleration in supernova remnant SN 1006. Astron. J. 2013;145(4).
http://dx.doi.org/10.1088/0004-6256/145/4/104