Response to "comment on "slow-mode shock candidate in the Jovian magnetosheath" by Bebesi et al."

Z. Bebesi, K. Szegö, A. Balogh, N. Krupp, G. Erdős, A. M. Rymer, G. R. Lewis, W. S. Kurth, D. T. Young, M. K. Dougherty

Research output: Article

Abstract

Hubert and Samsonov addressed our paper published in early 2010 (Bebesi et al.; 2010) about a plasma event detected in the magnetosheath of Jupiter by the plasma instruments of the Cassini spacecraft. We proposed that the characteristics of the plasma parameter variations were consistent with a slow mode shock (SMS). As our title indicated, we claimed only that the event was a possible "candidate" for an SMS according to our data, which had some restrictions as discussed in the paper. As to the origin, we proposed the following: since there was a crossing of the then highly tilted Heliospheric Current Sheet in less than two days before the event, it might have played a role in initiating the shock front. We highly appreciate the opinion of the authors, but they do not point out any hard fact that would exclude the possibility of the scenario we suggested.

Original languageEnglish
Pages (from-to)445-446
Number of pages2
JournalPlanetary and Space Science
Volume59
Issue number5-6
DOIs
Publication statusPublished - ápr. 2011

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magnetosheath
shock
plasma
shock fronts
current sheets
Jupiter (planet)
Jupiter
constrictions
spacecraft

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics

Cite this

Response to "comment on "slow-mode shock candidate in the Jovian magnetosheath" by Bebesi et al.". / Bebesi, Z.; Szegö, K.; Balogh, A.; Krupp, N.; Erdős, G.; Rymer, A. M.; Lewis, G. R.; Kurth, W. S.; Young, D. T.; Dougherty, M. K.

In: Planetary and Space Science, Vol. 59, No. 5-6, 04.2011, p. 445-446.

Research output: Article

Bebesi, Z, Szegö, K, Balogh, A, Krupp, N, Erdős, G, Rymer, AM, Lewis, GR, Kurth, WS, Young, DT & Dougherty, MK 2011, 'Response to "comment on "slow-mode shock candidate in the Jovian magnetosheath" by Bebesi et al."', Planetary and Space Science, vol. 59, no. 5-6, pp. 445-446. https://doi.org/10.1016/j.pss.2010.10.007
Bebesi, Z. ; Szegö, K. ; Balogh, A. ; Krupp, N. ; Erdős, G. ; Rymer, A. M. ; Lewis, G. R. ; Kurth, W. S. ; Young, D. T. ; Dougherty, M. K. / Response to "comment on "slow-mode shock candidate in the Jovian magnetosheath" by Bebesi et al.". In: Planetary and Space Science. 2011 ; Vol. 59, No. 5-6. pp. 445-446.
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abstract = "Hubert and Samsonov addressed our paper published in early 2010 (Bebesi et al.; 2010) about a plasma event detected in the magnetosheath of Jupiter by the plasma instruments of the Cassini spacecraft. We proposed that the characteristics of the plasma parameter variations were consistent with a slow mode shock (SMS). As our title indicated, we claimed only that the event was a possible {"}candidate{"} for an SMS according to our data, which had some restrictions as discussed in the paper. As to the origin, we proposed the following: since there was a crossing of the then highly tilted Heliospheric Current Sheet in less than two days before the event, it might have played a role in initiating the shock front. We highly appreciate the opinion of the authors, but they do not point out any hard fact that would exclude the possibility of the scenario we suggested.",
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AU - Bebesi, Z.

AU - Szegö, K.

AU - Balogh, A.

AU - Krupp, N.

AU - Erdős, G.

AU - Rymer, A. M.

AU - Lewis, G. R.

AU - Kurth, W. S.

AU - Young, D. T.

AU - Dougherty, M. K.

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AB - Hubert and Samsonov addressed our paper published in early 2010 (Bebesi et al.; 2010) about a plasma event detected in the magnetosheath of Jupiter by the plasma instruments of the Cassini spacecraft. We proposed that the characteristics of the plasma parameter variations were consistent with a slow mode shock (SMS). As our title indicated, we claimed only that the event was a possible "candidate" for an SMS according to our data, which had some restrictions as discussed in the paper. As to the origin, we proposed the following: since there was a crossing of the then highly tilted Heliospheric Current Sheet in less than two days before the event, it might have played a role in initiating the shock front. We highly appreciate the opinion of the authors, but they do not point out any hard fact that would exclude the possibility of the scenario we suggested.

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KW - Shock waves

KW - Slow-mode shocks

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