Shock location and CME 3D reconstruction of a solar type II radio burst with LOFAR

P. Zucca; D. E. Morosan; A. P. Rouillard; R. Fallows; P. T. Gallagher; J. Magdalenic; K. L. Klein; G. Mann; C. Vocks; E. P. Carley; M. M. Bisi; E. P. Kontar; H. Rothkaehl; B. Dabrowski; A. Krankowski; J. Anderson; A. Asgekar; M. E. Bell; M. J. Bentum; P. Best; R. Blaauw; F. Breitling; J. W. Broderick; W. N. Brouw; M. Brüggen; H. R. Butcher; B. Ciardi; E. De Geus; A. Deller; S. Duscha; J. Eislöffel; M. A. Garrett; J. M. Grießmeier; A. W. Gunst; G. Heald; M. Hoeft; J. Hörandel; M. Iacobelli; E. Juette; A. Karastergiou; J. Van Leeuwen; D. McKay-Bukowski; H. Mulder; H. Munk; A. Nelles; E. Orru; H. Paas; V. N. Pandey; R. Pekal; R. Pizzo; A. G. Polatidis; W. Reich; A. Rowlinson; D. J. Schwarz; A. Shulevski; J. Sluman; O. Smirnov; C. Sobey; M. Soida; S. Thoudam; M. C. Toribio; R. Vermeulen; R. J. Van Weeren; O. Wucknitz; P. Zarka

doi:10.1051/0004-6361/201732308

Shock location and CME 3D reconstruction of a solar type II radio burst with LOFAR

P. Zucca
, D. E. Morosan
, A. P. Rouillard
, R. Fallows
, P. T. Gallagher
, J. Magdalenic
, K. L. Klein
, G. Mann
, C. Vocks
, E. P. Carley
, M. M. Bisi
, E. P. Kontar
, H. Rothkaehl
, B. Dabrowski
, A. Krankowski
, J. Anderson
, A. Asgekar
, M. E. Bell
, M. J. Bentum
, P. Best

R. Blaauw, F. Breitling, J. W. Broderick, W. N. Brouw, M. Brüggen, H. R. Butcher, B. Ciardi, E. De Geus, A. Deller, S. Duscha, J. Eislöffel, M. A. Garrett, J. M. Grießmeier, A. W. Gunst, G. Heald, M. Hoeft, J. Hörandel, M. Iacobelli, E. Juette, A. Karastergiou, J. Van Leeuwen, D. McKay-Bukowski, H. Mulder, H. Munk, A. Nelles, E. Orru, H. Paas, V. N. Pandey, R. Pekal, R. Pizzo, A. G. Polatidis, W. Reich, A. Rowlinson, D. J. Schwarz, A. Shulevski, J. Sluman, O. Smirnov, C. Sobey, M. Soida, S. Thoudam, M. C. Toribio, R. Vermeulen, R. J. Van Weeren, O. Wucknitz, P. Zarka

Physics

Netherlands Institute of Radio Astronomy (ASTRON)
Trinity College Dublin
Institut de Recherche en Astrophysique et Planétologie (IRAP)
Observatoire de Paris
Leibniz-Institut für Astrophysik Potsdam (AIP)
Royal Observatory of Belgium
RAL Space
University of Glasgow
Space Research Centre of the Polish Academy of Science
University of Warmia and Mazury in Olsztyn
GFZ German Research Centre for Geosciences
Shell Technology Center
University of Technology Sydney
Eindhoven University of Technology
University of Edinburgh, Institute for Astronomy
University of Groningen
Universität Hamburg
Australian National University
Max Planck Institute for Astrophysics
SmarterVision BV
Swinburne University of Technology
Thüringer Landessternwarte
University of Manchester
Leiden University
LPC2E - Univ. d'Orléans/cnrs
Station de Radioastronomie de Nancay
CSIRO Astronomy and Space Science
Radboud University Nijmegen
University of Bochum
University of Oxford
University of Amsterdam
The Arctic University of Norway (UiT)
Harwell Science and Innovation Campus
University of California-Irvine
University Groningen
Poznan Supercomputing and Networking Center (PCSS)
Max-Planck-Institut für Radioastronomie
Universität Bielefeld
Rhodes University
SKA South Africa
Curtin University
Jagiellonian University

Research output: Contribution to journal › Article › peer-review

74 Scopus citations

Abstract

Context. Type II radio bursts are evidence of shocks in the solar atmosphere and inner heliosphere that emit radio waves ranging from sub-meter to kilometer lengths. These shocks may be associated with coronal mass ejections (CMEs) and reach speeds higher than the local magnetosonic speed. Radio imaging of decameter wavelengths (20-90 MHz) is now possible with the Low Frequency Array (LOFAR), opening a new radio window in which to study coronal shocks that leave the inner solar corona and enter the interplanetary medium and to understand their association with CMEs. Aims. To this end, we study a coronal shock associated with a CME and type II radio burst to determine the locations at which the radio emission is generated, and we investigate the origin of the band-splitting phenomenon. Methods. Thetype II shock source-positions and spectra were obtained using 91 simultaneous tied-array beams of LOFAR, and the CME was observed by the Large Angle and Spectrometric Coronagraph (LASCO) on board the Solar and Heliospheric Observatory (SOHO) and by the COR2A coronagraph of the SECCHI instruments on board the Solar Terrestrial Relation Observatory(STEREO). The 3D structure was inferred using triangulation of the coronographic observations. Coronal magnetic fields were obtained from a 3D magnetohydrodynamics (MHD) polytropic model using the photospheric fields measured by the Heliospheric Imager (HMI) on board the Solar Dynamic Observatory (SDO) as lower boundary. Results. The type II radio source of the coronal shock observed between 50 and 70 MHz was found to be located at the expanding flank of the CME, where the shock geometry is quasi-perpendicular with θ_Bn ~ 70°. The type II radio burst showed first and second harmonic emission; the second harmonic source was cospatial with the first harmonic source to within the observational uncertainty. This suggests that radio wave propagation does not alter the apparent location of the harmonic source. The sources of the two split bands were also found to be cospatial within the observational uncertainty, in agreement with the interpretation that split bands are simultaneous radio emission from upstream and downstream of the shock front. The fast magnetosonic Mach number derived from this interpretation was found to lie in the range 1.3-1.5. The fast magnetosonic Mach numbers derived from modelling the CME and the coronal magnetic field around the type II source were found to lie in the range 1.4-1.6.

Original language	British English
Article number	A89
Journal	Astronomy and Astrophysics
Volume	615
DOIs	https://doi.org/10.1051/0004-6361/201732308
State	Published - 1 Jul 2018

Keywords

Sun: corona
Sun: coronal mass ejections (CMEs)
Sun: radio radiation

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10.1051/0004-6361/201732308

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Zucca, P., Morosan, D. E., Rouillard, A. P., Fallows, R., Gallagher, P. T., Magdalenic, J., Klein, K. L., Mann, G., Vocks, C., Carley, E. P., Bisi, M. M., Kontar, E. P., Rothkaehl, H., Dabrowski, B., Krankowski, A., Anderson, J., Asgekar, A., Bell, M. E., Bentum, M. J., ... Zarka, P. (2018). Shock location and CME 3D reconstruction of a solar type II radio burst with LOFAR. Astronomy and Astrophysics, 615, Article A89. https://doi.org/10.1051/0004-6361/201732308

@article{bcab770036344c44b684c650d3e4d276,

title = "Shock location and CME 3D reconstruction of a solar type II radio burst with LOFAR",

abstract = "Context. Type II radio bursts are evidence of shocks in the solar atmosphere and inner heliosphere that emit radio waves ranging from sub-meter to kilometer lengths. These shocks may be associated with coronal mass ejections (CMEs) and reach speeds higher than the local magnetosonic speed. Radio imaging of decameter wavelengths (20-90 MHz) is now possible with the Low Frequency Array (LOFAR), opening a new radio window in which to study coronal shocks that leave the inner solar corona and enter the interplanetary medium and to understand their association with CMEs. Aims. To this end, we study a coronal shock associated with a CME and type II radio burst to determine the locations at which the radio emission is generated, and we investigate the origin of the band-splitting phenomenon. Methods. Thetype II shock source-positions and spectra were obtained using 91 simultaneous tied-array beams of LOFAR, and the CME was observed by the Large Angle and Spectrometric Coronagraph (LASCO) on board the Solar and Heliospheric Observatory (SOHO) and by the COR2A coronagraph of the SECCHI instruments on board the Solar Terrestrial Relation Observatory(STEREO). The 3D structure was inferred using triangulation of the coronographic observations. Coronal magnetic fields were obtained from a 3D magnetohydrodynamics (MHD) polytropic model using the photospheric fields measured by the Heliospheric Imager (HMI) on board the Solar Dynamic Observatory (SDO) as lower boundary. Results. The type II radio source of the coronal shock observed between 50 and 70 MHz was found to be located at the expanding flank of the CME, where the shock geometry is quasi-perpendicular with θBn \textasciitilde{} 70°. The type II radio burst showed first and second harmonic emission; the second harmonic source was cospatial with the first harmonic source to within the observational uncertainty. This suggests that radio wave propagation does not alter the apparent location of the harmonic source. The sources of the two split bands were also found to be cospatial within the observational uncertainty, in agreement with the interpretation that split bands are simultaneous radio emission from upstream and downstream of the shock front. The fast magnetosonic Mach number derived from this interpretation was found to lie in the range 1.3-1.5. The fast magnetosonic Mach numbers derived from modelling the CME and the coronal magnetic field around the type II source were found to lie in the range 1.4-1.6.",

keywords = "Sun: corona, Sun: coronal mass ejections (CMEs), Sun: radio radiation",

author = "P. Zucca and Morosan, \{D. E.\} and Rouillard, \{A. P.\} and R. Fallows and Gallagher, \{P. T.\} and J. Magdalenic and Klein, \{K. L.\} and G. Mann and C. Vocks and Carley, \{E. P.\} and Bisi, \{M. M.\} and Kontar, \{E. P.\} and H. Rothkaehl and B. Dabrowski and A. Krankowski and J. Anderson and A. Asgekar and Bell, \{M. E.\} and Bentum, \{M. J.\} and P. Best and R. Blaauw and F. Breitling and Broderick, \{J. W.\} and Brouw, \{W. N.\} and M. Br{\"u}ggen and Butcher, \{H. R.\} and B. Ciardi and \{De Geus\}, E. and A. Deller and S. Duscha and J. Eisl{\"o}ffel and Garrett, \{M. A.\} and Grie{\ss}meier, \{J. M.\} and Gunst, \{A. W.\} and G. Heald and M. Hoeft and J. H{\"o}randel and M. Iacobelli and E. Juette and A. Karastergiou and \{Van Leeuwen\}, J. and D. McKay-Bukowski and H. Mulder and H. Munk and A. Nelles and E. Orru and H. Paas and Pandey, \{V. N.\} and R. Pekal and R. Pizzo and Polatidis, \{A. G.\} and W. Reich and A. Rowlinson and Schwarz, \{D. J.\} and A. Shulevski and J. Sluman and O. Smirnov and C. Sobey and M. Soida and S. Thoudam and Toribio, \{M. C.\} and R. Vermeulen and \{Van Weeren\}, \{R. J.\} and O. Wucknitz and P. Zarka",

note = "Funding Information: tional LOFAR Telescope (ILT). LOFAR (van Haarlem et al. 2013) is the Low Frequency Array designed and constructed by ASTRON. It has facilities in several countries that are owned by various parties (each with their own funding sources), and that are collectively operated by the ILT foundation under a joint scientific policy. We are also grateful to the STEREO, SDO, and LASCO team for the data access. A. P. Rouillard acknowledges funding from the French “Agence Nationale de la Recherche” under contract number ANR-17-CE31-0006-01. Publisher Copyright: {\textcopyright} ESO 2018.",

year = "2018",

month = jul,

day = "1",

doi = "10.1051/0004-6361/201732308",

language = "British English",

volume = "615",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

}

Zucca, P, Morosan, DE, Rouillard, AP, Fallows, R, Gallagher, PT, Magdalenic, J, Klein, KL, Mann, G, Vocks, C, Carley, EP, Bisi, MM, Kontar, EP, Rothkaehl, H, Dabrowski, B, Krankowski, A, Anderson, J, Asgekar, A, Bell, ME, Bentum, MJ, Best, P, Blaauw, R, Breitling, F, Broderick, JW, Brouw, WN, Brüggen, M, Butcher, HR, Ciardi, B, De Geus, E, Deller, A, Duscha, S, Eislöffel, J, Garrett, MA, Grießmeier, JM, Gunst, AW, Heald, G, Hoeft, M, Hörandel, J, Iacobelli, M, Juette, E, Karastergiou, A, Van Leeuwen, J, McKay-Bukowski, D, Mulder, H, Munk, H, Nelles, A, Orru, E, Paas, H, Pandey, VN, Pekal, R, Pizzo, R, Polatidis, AG, Reich, W, Rowlinson, A, Schwarz, DJ, Shulevski, A, Sluman, J, Smirnov, O, Sobey, C, Soida, M, Thoudam, S, Toribio, MC, Vermeulen, R, Van Weeren, RJ, Wucknitz, O & Zarka, P 2018, 'Shock location and CME 3D reconstruction of a solar type II radio burst with LOFAR', Astronomy and Astrophysics, vol. 615, A89. https://doi.org/10.1051/0004-6361/201732308

TY - JOUR

T1 - Shock location and CME 3D reconstruction of a solar type II radio burst with LOFAR

AU - Zucca, P.

AU - Morosan, D. E.

AU - Rouillard, A. P.

AU - Fallows, R.

AU - Gallagher, P. T.

AU - Magdalenic, J.

AU - Klein, K. L.

AU - Mann, G.

AU - Vocks, C.

AU - Carley, E. P.

AU - Bisi, M. M.

AU - Kontar, E. P.

AU - Rothkaehl, H.

AU - Dabrowski, B.

AU - Krankowski, A.

AU - Anderson, J.

AU - Asgekar, A.

AU - Bell, M. E.

AU - Bentum, M. J.

AU - Best, P.

AU - Blaauw, R.

AU - Breitling, F.

AU - Broderick, J. W.

AU - Brouw, W. N.

AU - Brüggen, M.

AU - Butcher, H. R.

AU - Ciardi, B.

AU - De Geus, E.

AU - Deller, A.

AU - Duscha, S.

AU - Eislöffel, J.

AU - Garrett, M. A.

AU - Grießmeier, J. M.

AU - Gunst, A. W.

AU - Heald, G.

AU - Hoeft, M.

AU - Hörandel, J.

AU - Iacobelli, M.

AU - Juette, E.

AU - Karastergiou, A.

AU - Van Leeuwen, J.

AU - McKay-Bukowski, D.

AU - Mulder, H.

AU - Munk, H.

AU - Nelles, A.

AU - Orru, E.

AU - Paas, H.

AU - Pandey, V. N.

AU - Pekal, R.

AU - Pizzo, R.

AU - Polatidis, A. G.

AU - Reich, W.

AU - Rowlinson, A.

AU - Schwarz, D. J.

AU - Shulevski, A.

AU - Sluman, J.

AU - Smirnov, O.

AU - Sobey, C.

AU - Soida, M.

AU - Thoudam, S.

AU - Toribio, M. C.

AU - Vermeulen, R.

AU - Van Weeren, R. J.

AU - Wucknitz, O.

AU - Zarka, P.

N1 - Funding Information: tional LOFAR Telescope (ILT). LOFAR (van Haarlem et al. 2013) is the Low Frequency Array designed and constructed by ASTRON. It has facilities in several countries that are owned by various parties (each with their own funding sources), and that are collectively operated by the ILT foundation under a joint scientific policy. We are also grateful to the STEREO, SDO, and LASCO team for the data access. A. P. Rouillard acknowledges funding from the French “Agence Nationale de la Recherche” under contract number ANR-17-CE31-0006-01. Publisher Copyright: © ESO 2018.

PY - 2018/7/1

Y1 - 2018/7/1

N2 - Context. Type II radio bursts are evidence of shocks in the solar atmosphere and inner heliosphere that emit radio waves ranging from sub-meter to kilometer lengths. These shocks may be associated with coronal mass ejections (CMEs) and reach speeds higher than the local magnetosonic speed. Radio imaging of decameter wavelengths (20-90 MHz) is now possible with the Low Frequency Array (LOFAR), opening a new radio window in which to study coronal shocks that leave the inner solar corona and enter the interplanetary medium and to understand their association with CMEs. Aims. To this end, we study a coronal shock associated with a CME and type II radio burst to determine the locations at which the radio emission is generated, and we investigate the origin of the band-splitting phenomenon. Methods. Thetype II shock source-positions and spectra were obtained using 91 simultaneous tied-array beams of LOFAR, and the CME was observed by the Large Angle and Spectrometric Coronagraph (LASCO) on board the Solar and Heliospheric Observatory (SOHO) and by the COR2A coronagraph of the SECCHI instruments on board the Solar Terrestrial Relation Observatory(STEREO). The 3D structure was inferred using triangulation of the coronographic observations. Coronal magnetic fields were obtained from a 3D magnetohydrodynamics (MHD) polytropic model using the photospheric fields measured by the Heliospheric Imager (HMI) on board the Solar Dynamic Observatory (SDO) as lower boundary. Results. The type II radio source of the coronal shock observed between 50 and 70 MHz was found to be located at the expanding flank of the CME, where the shock geometry is quasi-perpendicular with θBn ~ 70°. The type II radio burst showed first and second harmonic emission; the second harmonic source was cospatial with the first harmonic source to within the observational uncertainty. This suggests that radio wave propagation does not alter the apparent location of the harmonic source. The sources of the two split bands were also found to be cospatial within the observational uncertainty, in agreement with the interpretation that split bands are simultaneous radio emission from upstream and downstream of the shock front. The fast magnetosonic Mach number derived from this interpretation was found to lie in the range 1.3-1.5. The fast magnetosonic Mach numbers derived from modelling the CME and the coronal magnetic field around the type II source were found to lie in the range 1.4-1.6.

AB - Context. Type II radio bursts are evidence of shocks in the solar atmosphere and inner heliosphere that emit radio waves ranging from sub-meter to kilometer lengths. These shocks may be associated with coronal mass ejections (CMEs) and reach speeds higher than the local magnetosonic speed. Radio imaging of decameter wavelengths (20-90 MHz) is now possible with the Low Frequency Array (LOFAR), opening a new radio window in which to study coronal shocks that leave the inner solar corona and enter the interplanetary medium and to understand their association with CMEs. Aims. To this end, we study a coronal shock associated with a CME and type II radio burst to determine the locations at which the radio emission is generated, and we investigate the origin of the band-splitting phenomenon. Methods. Thetype II shock source-positions and spectra were obtained using 91 simultaneous tied-array beams of LOFAR, and the CME was observed by the Large Angle and Spectrometric Coronagraph (LASCO) on board the Solar and Heliospheric Observatory (SOHO) and by the COR2A coronagraph of the SECCHI instruments on board the Solar Terrestrial Relation Observatory(STEREO). The 3D structure was inferred using triangulation of the coronographic observations. Coronal magnetic fields were obtained from a 3D magnetohydrodynamics (MHD) polytropic model using the photospheric fields measured by the Heliospheric Imager (HMI) on board the Solar Dynamic Observatory (SDO) as lower boundary. Results. The type II radio source of the coronal shock observed between 50 and 70 MHz was found to be located at the expanding flank of the CME, where the shock geometry is quasi-perpendicular with θBn ~ 70°. The type II radio burst showed first and second harmonic emission; the second harmonic source was cospatial with the first harmonic source to within the observational uncertainty. This suggests that radio wave propagation does not alter the apparent location of the harmonic source. The sources of the two split bands were also found to be cospatial within the observational uncertainty, in agreement with the interpretation that split bands are simultaneous radio emission from upstream and downstream of the shock front. The fast magnetosonic Mach number derived from this interpretation was found to lie in the range 1.3-1.5. The fast magnetosonic Mach numbers derived from modelling the CME and the coronal magnetic field around the type II source were found to lie in the range 1.4-1.6.

KW - Sun: corona

KW - Sun: coronal mass ejections (CMEs)

KW - Sun: radio radiation

UR - https://www.scopus.com/pages/publications/85056140524

U2 - 10.1051/0004-6361/201732308

DO - 10.1051/0004-6361/201732308

M3 - Article

AN - SCOPUS:85056140524

SN - 0004-6361

VL - 615

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A89

ER -

Shock location and CME 3D reconstruction of a solar type II radio burst with LOFAR

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Keywords

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