Photospheric Response to an Ellerman Bomb-like Event - An Analogy of Sunrise/IMaX Observations and MHD Simulations

S. Danilovic; S. K. Solanki; P. Barthol; A. Gandorfer; L. Gizon; J. Hirzberger; T. L. Riethmüller; M. Van Noort; J. Blanco Rodríguez; J. C. Del Toro Iniesta; D. Orozco Suárez; W. Schmidt; V. Martínez Pillet; M. Knölker

doi:10.3847/1538-4365/229/1/5

Photospheric Response to an Ellerman Bomb-like Event - An Analogy of Sunrise/IMaX Observations and MHD Simulations

S. Danilovic, S. K. Solanki, P. Barthol, A. Gandorfer, L. Gizon, J. Hirzberger, T. L. Riethmüller, M. Van Noort, J. Blanco Rodríguez, J. C. Del Toro Iniesta, D. Orozco Suárez, W. Schmidt, V. Martínez Pillet, M. Knölker

Center for Space Science

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

Abstract

Ellerman Bombs are signatures of magnetic reconnection, which is an important physical process in the solar atmosphere. How and where they occur is a subject of debate. In this paper, we analyze Sunrise/IMaX data, along with 3D MHD simulations that aim to reproduce the exact scenario proposed for the formation of these features. Although the observed event seems to be more dynamic and violent than the simulated one, simulations clearly confirm the basic scenario for the production of EBs. The simulations also reveal the full complexity of the underlying process. The simulated observations show that the Fe i 525.02 nm line gives no information on the height where reconnection takes place. It can only give clues about the heating in the aftermath of the reconnection. However, the information on the magnetic field vector and velocity at this spatial resolution is extremely valuable because it shows what numerical models miss and how they can be improved.

Original language	English (US)
Article number	5
Journal	Astrophysical Journal, Supplement Series
Volume	229
Issue number	1
DOIs	https://doi.org/10.3847/1538-4365/229/1/5
State	Published - Mar 2017

Keywords

Sun: activity
Sun: magnetic fields
Sun: photosphere
techniques: photometric

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.3847/1538-4365/229/1/5

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Danilovic, S., Solanki, S. K., Barthol, P., Gandorfer, A., Gizon, L., Hirzberger, J., Riethmüller, T. L., Van Noort, M., Rodríguez, J. B., Del Toro Iniesta, J. C., Suárez, D. O., Schmidt, W., Pillet, V. M., & Knölker, M. (2017). Photospheric Response to an Ellerman Bomb-like Event - An Analogy of Sunrise/IMaX Observations and MHD Simulations. Astrophysical Journal, Supplement Series, 229(1), Article 5. https://doi.org/10.3847/1538-4365/229/1/5

Danilovic, S, Solanki, SK, Barthol, P, Gandorfer, A, Gizon, L, Hirzberger, J, Riethmüller, TL, Van Noort, M, Rodríguez, JB, Del Toro Iniesta, JC, Suárez, DO, Schmidt, W, Pillet, VM & Knölker, M 2017, 'Photospheric Response to an Ellerman Bomb-like Event - An Analogy of Sunrise/IMaX Observations and MHD Simulations', Astrophysical Journal, Supplement Series, vol. 229, no. 1, 5. https://doi.org/10.3847/1538-4365/229/1/5

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abstract = "Ellerman Bombs are signatures of magnetic reconnection, which is an important physical process in the solar atmosphere. How and where they occur is a subject of debate. In this paper, we analyze Sunrise/IMaX data, along with 3D MHD simulations that aim to reproduce the exact scenario proposed for the formation of these features. Although the observed event seems to be more dynamic and violent than the simulated one, simulations clearly confirm the basic scenario for the production of EBs. The simulations also reveal the full complexity of the underlying process. The simulated observations show that the Fe i 525.02 nm line gives no information on the height where reconnection takes place. It can only give clues about the heating in the aftermath of the reconnection. However, the information on the magnetic field vector and velocity at this spatial resolution is extremely valuable because it shows what numerical models miss and how they can be improved.",

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author = "S. Danilovic and Solanki, {S. K.} and P. Barthol and A. Gandorfer and L. Gizon and J. Hirzberger and Riethm{\"u}ller, {T. L.} and {Van Noort}, M. and Rodr{\'i}guez, {J. Blanco} and {Del Toro Iniesta}, {J. C.} and Su{\'a}rez, {D. Orozco} and W. Schmidt and Pillet, {V. Mart{\'i}nez} and M. Kn{\"o}lker",

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doi = "10.3847/1538-4365/229/1/5",

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AU - Danilovic, S.

AU - Solanki, S. K.

AU - Barthol, P.

AU - Gandorfer, A.

AU - Gizon, L.

AU - Hirzberger, J.

AU - Riethmüller, T. L.

AU - Van Noort, M.

AU - Rodríguez, J. Blanco

AU - Del Toro Iniesta, J. C.

AU - Suárez, D. Orozco

AU - Schmidt, W.

AU - Pillet, V. Martínez

AU - Knölker, M.

PY - 2017/3

Y1 - 2017/3

N2 - Ellerman Bombs are signatures of magnetic reconnection, which is an important physical process in the solar atmosphere. How and where they occur is a subject of debate. In this paper, we analyze Sunrise/IMaX data, along with 3D MHD simulations that aim to reproduce the exact scenario proposed for the formation of these features. Although the observed event seems to be more dynamic and violent than the simulated one, simulations clearly confirm the basic scenario for the production of EBs. The simulations also reveal the full complexity of the underlying process. The simulated observations show that the Fe i 525.02 nm line gives no information on the height where reconnection takes place. It can only give clues about the heating in the aftermath of the reconnection. However, the information on the magnetic field vector and velocity at this spatial resolution is extremely valuable because it shows what numerical models miss and how they can be improved.

AB - Ellerman Bombs are signatures of magnetic reconnection, which is an important physical process in the solar atmosphere. How and where they occur is a subject of debate. In this paper, we analyze Sunrise/IMaX data, along with 3D MHD simulations that aim to reproduce the exact scenario proposed for the formation of these features. Although the observed event seems to be more dynamic and violent than the simulated one, simulations clearly confirm the basic scenario for the production of EBs. The simulations also reveal the full complexity of the underlying process. The simulated observations show that the Fe i 525.02 nm line gives no information on the height where reconnection takes place. It can only give clues about the heating in the aftermath of the reconnection. However, the information on the magnetic field vector and velocity at this spatial resolution is extremely valuable because it shows what numerical models miss and how they can be improved.

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KW - Sun: magnetic fields

KW - Sun: photosphere

KW - techniques: photometric

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Photospheric Response to an Ellerman Bomb-like Event - An Analogy of Sunrise/IMaX Observations and MHD Simulations

Abstract

Keywords

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