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Your search keyword '"Hassler, D. M."' showing total 17 results
Start Over Author "Hassler, D. M." Publication Type Electronic Resources
17 results on '"Hassler, D. M."'

1. SPICE Connection Mosaics to link the Sun's surface and the heliosphere

Author

Varesano, T., Hassler, D. M., Prado, N. Zambrana, Plowman, J., Del Zanna, G., Parenti, S., Mason, H. E., Giunta, A., Auchere, F., Carlsson, M., Fludra, A., Peter, H., Muller, D., Williams, D., Cuadrado, R. Aznar, Barczynski, K., Buchlin, E., Caldwell, M., Fredvik, T., Grundy, T., Guest, S., Harra, L., Janvier, M., Kucera, T., Leeks, S., Schmutz, W., Schuehle, U., Sidher, S., Teriaca, L., Thompson, W., Yardley, S. L., Varesano, T., Hassler, D. M., Prado, N. Zambrana, Plowman, J., Del Zanna, G., Parenti, S., Mason, H. E., Giunta, A., Auchere, F., Carlsson, M., Fludra, A., Peter, H., Muller, D., Williams, D., Cuadrado, R. Aznar, Barczynski, K., Buchlin, E., Caldwell, M., Fredvik, T., Grundy, T., Guest, S., Harra, L., Janvier, M., Kucera, T., Leeks, S., Schmutz, W., Schuehle, U., Sidher, S., Teriaca, L., Thompson, W., and Yardley, S. L.

Abstract

We present an analysis of the first connection mosaic made by the SPICE instrument on board of the ESA / NASA Solar Orbiter mission on March 2nd, 2022. The data will be used to map coronal composition that will be compared with in-situ measurements taken by SWA/HIS to establish the coronal origin of the solar wind plasma observed at Solar Orbiter. The SPICE spectral lines were chosen to have varying sensitivity to the First Ionization Potential (FIP) effect, and therefore the radiances of the spectral lines will vary significantly depending on whether the elemental composition is coronal or photospheric. We investigate the link between the behavior of sulfur with the hypothesis that Alfv\'en waves drive FIP fractionation above the chromosphere. We perform temperature diagnostics using line ratios and Emission Measure (EM) loci, and compute relative FIP biases using three different approaches (two line ratio (2LR), ratios of linear combinations of spectral lines (LCR), and differential emission measure (DEM) inversion) to perform composition diagnostics in the corona. We then compare the SPICE composition analysis and EUI data of the potential solar wind source regions to the SWA / HIS data products. Radiance maps are extracted from SPICE spectral data cubes, with values matching previous observations. We find isothermal plasma of around LogT = 5.8 for the active region loops targeted, and that higher FIP-bias values are present at the footpoints of the coronal loops associated with two active regions. Comparing the results with the SWA/HIS data products encourages us to think that Solar Orbiter was connected to a source of slow solar wind during this observation campaign. We demonstrate FIP fractionation in observations of the upper chromosphere and transition region, emphasized by the behavior of the intermediate-FIP element sulfur., Comment: 20 pages, 19 figures, submitted to A&A on August 3rd, accepted on February 12th, 2024

Published
2023

2. The Multiview Observatory for Solar Terrestrial Science (MOST)

Author

Gopalswamy, N., Christe, S., Fung, S. F., Gong, Q., Gruesbeck, J. R., Jian, L. K., Kanekal, S. G., Kay, C., Kucera, T. A., Leake, J. E., Li, L., Makela, P., Nikulla, P., Reginald, N. L., Shih, A., Tadikonda, S. K., Viall, N., Wilson III, L. B., Yashiro, S., Golub, L., DeLuca, E., Reeves, K., Sterling, A. C., Winebarger, A. R., DeForest, C., Hassler, D. M., Seaton, D. B., Desai, M. I., Mokashi, P. S., Lazio, J., Jensen, E. A., Manchester, W. B., Sachdeva, N., Wood, B., Kooi, J., Hess, P., Wexler, D. B., Bale, S. D., Krucker, S., Hurlburt, N., DeRosa, M., Gosain, S., Jain, K., Kholikov, S., Petrie, G. J. D., Pevtsov, A., Tripathy, S. C., Zhao, J., Scherrer, P. H., Rajaguru, S. P., Woods, T., Kenney, M., Zhang, J., Scolini, C., Cho, K. S., Park, Y. D., Jackson, B. V., Gopalswamy, N., Christe, S., Fung, S. F., Gong, Q., Gruesbeck, J. R., Jian, L. K., Kanekal, S. G., Kay, C., Kucera, T. A., Leake, J. E., Li, L., Makela, P., Nikulla, P., Reginald, N. L., Shih, A., Tadikonda, S. K., Viall, N., Wilson III, L. B., Yashiro, S., Golub, L., DeLuca, E., Reeves, K., Sterling, A. C., Winebarger, A. R., DeForest, C., Hassler, D. M., Seaton, D. B., Desai, M. I., Mokashi, P. S., Lazio, J., Jensen, E. A., Manchester, W. B., Sachdeva, N., Wood, B., Kooi, J., Hess, P., Wexler, D. B., Bale, S. D., Krucker, S., Hurlburt, N., DeRosa, M., Gosain, S., Jain, K., Kholikov, S., Petrie, G. J. D., Pevtsov, A., Tripathy, S. C., Zhao, J., Scherrer, P. H., Rajaguru, S. P., Woods, T., Kenney, M., Zhang, J., Scolini, C., Cho, K. S., Park, Y. D., and Jackson, B. V.

Abstract

We report on a study of the Multiview Observatory for Solar Terrestrial Science (MOST) mission that will provide comprehensive imagery and time series data needed to understand the magnetic connection between the solar interior and the solar atmosphere/inner heliosphere. MOST will build upon the successes of SOHO and STEREO missions with new views of the Sun and enhanced instrument capabilities. This article is based on a study conducted at NASA Goddard Space Flight Center that determined the required instrument refinement, spacecraft accommodation, launch configuration, and flight dynamics for mission success. MOST is envisioned as the next generation great observatory positioned to obtain three-dimensional information of large-scale heliospheric structures such as coronal mass ejections, stream interaction regions, and the solar wind itself. The MOST mission consists of 2 pairs of spacecraft located in the vicinity of Sun-Earth Lagrange points L4 (MOST1, MOST3) and L5 (MOST2 and MOST4). The spacecraft stationed at L4 (MOST1) and L5 (MOST2) will each carry seven remote-sensing and three in-situ instrument suites, including a novel radio package known as the Faraday Effect Tracker of Coronal and Heliospheric structures (FETCH). MOST3 and MOST4 will carry only the FETCH instruments and are positioned at variable locations along the Earth orbit up to 20{\deg} ahead of L4 and 20{\deg} behind L5, respectively. FETCH will have polarized radio transmitters and receivers on all four spacecraft to measure the magnetic content of solar wind structures propagating from the Sun to Earth using the Faraday rotation technique. The MOST mission will be able to sample the magnetized plasma throughout the Sun-Earth connected space during the mission lifetime over a solar cycle., Comment: 42 pages, 19 figures, 8 tables, to appear in J. Atmospheric and Solar Terrestrial Physics

Published
2023

3. Empirical relations between the intensities of Lyman lines of H and He$^+$

Author

Gordino, M., Auchère, F., Vial, J. -C., Bocchialini, K., Hassler, D. M., Bando, T., Ishikawa, R., Kano, R., Kobayashi, K., Narukage, N., Bueno, J. Trujillo, Winebarger, A., Gordino, M., Auchère, F., Vial, J. -C., Bocchialini, K., Hassler, D. M., Bando, T., Ishikawa, R., Kano, R., Kobayashi, K., Narukage, N., Bueno, J. Trujillo, and Winebarger, A.

Abstract

Empirical relations between major UV and extreme UV spectral lines are one of the inputs for models of chromospheric and coronal spectral radiances and irradiances. They are also needed for the interpretation of some of the observations of the Solar Orbiter mission. We aim to determine an empirical relation between the intensities of the HI 121.6 nm and HeII 30.4 nm Lyman $\alpha$ lines. Images at 121.6 nm from the Chromospheric Lyman Alpha Spectro Polarimeter (CLASP) and Multiple XUV Imager (MXUVI) sounding rockets were co-registered with simultaneous images at 30.4 nm from the EIT and AIA orbital telescopes in order to derive a spatially resolved relationship between the intensities. We have obtained a relationship between the HI 121.6 nm and HeII 30.4 nm intensities that is valid for a wide range of solar features, intensities, and activity levels. Additional SUMER data have allowed the derivation of another relation between the HI 102.5 nm (Ly$\beta$) and HeII 30.4 nm lines for quiet-Sun regions. We combined these two relationships to obtain a Ly$\alpha$/Ly$\beta$ intensity ratio that is comparable to the few previously published results. The relationship between the HI 121.6~nm and HeII 30.4 nm lines is consistent with the one previously obtained using irradiance data. We have also observed that this relation is stable in time but that its accuracy depends on the spatial resolution of the observations. The derived Ly$\alpha$/Ly$\beta$ intensity ratio is also compatible with previous results.

Published
2022
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4. Empirical relations between the intensities of Lyman lines of H and He$^+$

Author

Gordino, M., Auchère, F., Vial, J. -C., Bocchialini, K., Hassler, D. M., Bando, T., Ishikawa, R., Kano, R., Kobayashi, K., Narukage, N., Bueno, J. Trujillo, Winebarger, A., Gordino, M., Auchère, F., Vial, J. -C., Bocchialini, K., Hassler, D. M., Bando, T., Ishikawa, R., Kano, R., Kobayashi, K., Narukage, N., Bueno, J. Trujillo, and Winebarger, A.

Abstract

Empirical relations between major UV and extreme UV spectral lines are one of the inputs for models of chromospheric and coronal spectral radiances and irradiances. They are also needed for the interpretation of some of the observations of the Solar Orbiter mission. We aim to determine an empirical relation between the intensities of the HI 121.6 nm and HeII 30.4 nm Lyman $\alpha$ lines. Images at 121.6 nm from the Chromospheric Lyman Alpha Spectro Polarimeter (CLASP) and Multiple XUV Imager (MXUVI) sounding rockets were co-registered with simultaneous images at 30.4 nm from the EIT and AIA orbital telescopes in order to derive a spatially resolved relationship between the intensities. We have obtained a relationship between the HI 121.6 nm and HeII 30.4 nm intensities that is valid for a wide range of solar features, intensities, and activity levels. Additional SUMER data have allowed the derivation of another relation between the HI 102.5 nm (Ly$\beta$) and HeII 30.4 nm lines for quiet-Sun regions. We combined these two relationships to obtain a Ly$\alpha$/Ly$\beta$ intensity ratio that is comparable to the few previously published results. The relationship between the HI 121.6~nm and HeII 30.4 nm lines is consistent with the one previously obtained using irradiance data. We have also observed that this relation is stable in time but that its accuracy depends on the spatial resolution of the observations. The derived Ly$\alpha$/Ly$\beta$ intensity ratio is also compatible with previous results.

Published
2022
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5. The Solar Orbiter Science Activity Plan : Translating solar and heliospheric physics questions into action

Author

Zouganelis, I., De Groof, A., Walsh, A. P., Williams, D. R., Mueller, D., St Cyr, O. C., Auchere, F., Berghmans, D., Fludra, A., Horbury, T. S., Howard, R. A., Krucker, S., Maksimovic, M., Owen, C. J., Rodriguez-Pacheco, J., Romoli, M., Solanki, S. K., Watson, C., Sanchez, L., Lefort, J., Osuna, P., Gilbert, H. R., Nieves-Chinchilla, T., Abbo, L., Alexandrova, O., Anastasiadis, A., Andretta, V., Antonucci, E., Appourchaux, T., Aran, A., Arge, C. N., Aulanier, G., Baker, D., Bale, S. D., Battaglia, M., Bellot Rubio, L., Bemporad, A., Berthomier, M., Bocchialini, K., Bonnin, X., Brun, A. S., Bruno, R., Buchlin, E., Buechner, J., Bucik, R., Carcaboso, F., Carr, R., Carrasco-Blazquez, I., Cecconi, B., Cernuda Cangas, I., Chen, C. H. K., Chitta, L. P., Chust, T., Dalmasse, K., D'Amicis, R., Da Deppo, V., De Marco, R., Dolei, S., Dolla, L., de Wit, T. Dudok, van Driel-Gesztelyi, L., Eastwood, J. P., Espinosa Lara, F., Etesi, L., Fedorov, A., Felix-Redondo, F., Fineschi, S., Fleck, B., Fontaine, D., Fox, N. J., Gandorfer, A., Genot, V., Georgoulis, M. K., Gissot, S., Giunta, A., Gizon, L., Gomez-Herrero, R., Gontikakis, C., Graham, G., Green, L., Grundy, T., Haberreiter, M., Harra, L. K., Hassler, D. M., Hirzberger, J., Ho, G. C., Hurford, G., Innes, D., Issautier, K., James, A. W., Janitzek, N., Janvier, M., Jeffrey, N., Jenkins, J., Khotyaintsev, Yuri, Klein, K. -L, Kontar, E. P., Kontogiannis, I., Krafft, C., Krasnoselskikh, V., Kretzschmar, M., Labrosse, N., Lagg, A., Landini, F., Lavraud, B., Leon, I., Lepri, S. T., Lewis, G. R., Liewer, P., Linker, J., Livi, S., Long, D. M., Louarn, P., Malandraki, O., Maloney, S., Martinez-Pillet, V., Martinovic, M., Masson, A., Matthews, S., Matteini, L., Meyer-Vernet, N., Moraitis, K., Morton, R. J., Musset, S., Nicolaou, G., Nindos, A., O'Brien, H., Orozco Suarez, D., Owens, M., Pancrazzi, M., Papaioannou, A., Parenti, S., Pariat, E., Patsourakos, S., Perrone, D., Peter, H., Pinto, R. F., Plainaki, C., Plettemeier, D., Plunkett, S. P., Raines, J. M., Raouafi, N., Reid, H., Retino, A., Rezeau, L., Rochus, P., Rodriguez, L., Rodriguez-Garcia, L., Roth, M., Rouillard, A. P., Sahraoui, F., Sasso, C., Schou, J., Schuehle, U., Sorriso-Valvo, L., Soucek, J., Spadaro, D., Stangalini, M., Stansby, D., Steller, M., Strugarek, A., Stverak, S., Susino, R., Telloni, D., Terasa, C., Teriaca, L., Toledo-Redondo, S., del Toro Iniesta, J. C., Tsiropoula, G., Tsounis, A., Tziotziou, K., Valentini, F., Vaivads, A., Vecchio, A., Velli, M., Verbeeck, C., Verdini, A., Verscharen, D., Vilmer, N., Vourlidas, A., Wicks, R., Wimmer-Schweingruber, R. F., Wiegelmann, T., Young, P. R., Zhukov, A. N., Zouganelis, I., De Groof, A., Walsh, A. P., Williams, D. R., Mueller, D., St Cyr, O. C., Auchere, F., Berghmans, D., Fludra, A., Horbury, T. S., Howard, R. A., Krucker, S., Maksimovic, M., Owen, C. J., Rodriguez-Pacheco, J., Romoli, M., Solanki, S. K., Watson, C., Sanchez, L., Lefort, J., Osuna, P., Gilbert, H. R., Nieves-Chinchilla, T., Abbo, L., Alexandrova, O., Anastasiadis, A., Andretta, V., Antonucci, E., Appourchaux, T., Aran, A., Arge, C. N., Aulanier, G., Baker, D., Bale, S. D., Battaglia, M., Bellot Rubio, L., Bemporad, A., Berthomier, M., Bocchialini, K., Bonnin, X., Brun, A. S., Bruno, R., Buchlin, E., Buechner, J., Bucik, R., Carcaboso, F., Carr, R., Carrasco-Blazquez, I., Cecconi, B., Cernuda Cangas, I., Chen, C. H. K., Chitta, L. P., Chust, T., Dalmasse, K., D'Amicis, R., Da Deppo, V., De Marco, R., Dolei, S., Dolla, L., de Wit, T. Dudok, van Driel-Gesztelyi, L., Eastwood, J. P., Espinosa Lara, F., Etesi, L., Fedorov, A., Felix-Redondo, F., Fineschi, S., Fleck, B., Fontaine, D., Fox, N. J., Gandorfer, A., Genot, V., Georgoulis, M. K., Gissot, S., Giunta, A., Gizon, L., Gomez-Herrero, R., Gontikakis, C., Graham, G., Green, L., Grundy, T., Haberreiter, M., Harra, L. K., Hassler, D. M., Hirzberger, J., Ho, G. C., Hurford, G., Innes, D., Issautier, K., James, A. W., Janitzek, N., Janvier, M., Jeffrey, N., Jenkins, J., Khotyaintsev, Yuri, Klein, K. -L, Kontar, E. P., Kontogiannis, I., Krafft, C., Krasnoselskikh, V., Kretzschmar, M., Labrosse, N., Lagg, A., Landini, F., Lavraud, B., Leon, I., Lepri, S. T., Lewis, G. R., Liewer, P., Linker, J., Livi, S., Long, D. M., Louarn, P., Malandraki, O., Maloney, S., Martinez-Pillet, V., Martinovic, M., Masson, A., Matthews, S., Matteini, L., Meyer-Vernet, N., Moraitis, K., Morton, R. J., Musset, S., Nicolaou, G., Nindos, A., O'Brien, H., Orozco Suarez, D., Owens, M., Pancrazzi, M., Papaioannou, A., Parenti, S., Pariat, E., Patsourakos, S., Perrone, D., Peter, H., Pinto, R. F., Plainaki, C., Plettemeier, D., Plunkett, S. P., Raines, J. M., Raouafi, N., Reid, H., Retino, A., Rezeau, L., Rochus, P., Rodriguez, L., Rodriguez-Garcia, L., Roth, M., Rouillard, A. P., Sahraoui, F., Sasso, C., Schou, J., Schuehle, U., Sorriso-Valvo, L., Soucek, J., Spadaro, D., Stangalini, M., Stansby, D., Steller, M., Strugarek, A., Stverak, S., Susino, R., Telloni, D., Terasa, C., Teriaca, L., Toledo-Redondo, S., del Toro Iniesta, J. C., Tsiropoula, G., Tsounis, A., Tziotziou, K., Valentini, F., Vaivads, A., Vecchio, A., Velli, M., Verbeeck, C., Verdini, A., Verscharen, D., Vilmer, N., Vourlidas, A., Wicks, R., Wimmer-Schweingruber, R. F., Wiegelmann, T., Young, P. R., and Zhukov, A. N.

Abstract

Solar Orbiter is the first space mission observing the solar plasma both in situ and remotely, from a close distance, in and out of the ecliptic. The ultimate goal is to understand how the Sun produces and controls the heliosphere, filling the Solar System and driving the planetary environments. With six remote-sensing and four in-situ instrument suites, the coordination and planning of the operations are essential to address the following four top-level science questions: (1) What drives the solar wind and where does the coronal magnetic field originate?; (2) How do solar transients drive heliospheric variability?; (3) How do solar eruptions produce energetic particle radiation that fills the heliosphere?; (4) How does the solar dynamo work and drive connections between the Sun and the heliosphere? Maximising the mission's science return requires considering the characteristics of each orbit, including the relative position of the spacecraft to Earth (affecting downlink rates), trajectory events (such as gravitational assist manoeuvres), and the phase of the solar activity cycle. Furthermore, since each orbit's science telemetry will be downloaded over the course of the following orbit, science operations must be planned at mission level, rather than at the level of individual orbits. It is important to explore the way in which those science questions are translated into an actual plan of observations that fits into the mission, thus ensuring that no opportunities are missed. First, the overarching goals are broken down into specific, answerable questions along with the required observations and the so-called Science Activity Plan (SAP) is developed to achieve this. The SAP groups objectives that require similar observations into Solar Orbiter Observing Plans, resulting in a strategic, top-level view of the optimal opportunities for science observations during the mission lifetime. This allows for all four mission goals to be addressed. In this paper, we introduce

Published
2020
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6. The Solar Orbiter Science Activity Plan: translating solar and heliospheric physics questions into action

Author

Zouganelis, I., De Groof, A., Walsh, A. P., Williams, D. R., Mueller, D., Cyr, O. C. St, Auchere, F., Berghmans, D., Fludra, A., Horbury, T. S., Howard, R. A., Krucker, S., Maksimovic, M., Owen, C. J., Rodriiguez-Pacheco, J., Romoli, M., Solanki, S. K., Watson, C., Sanchez, L., Lefort, J., Osuna, P., Gilbert, H. R., Nieves-Chinchilla, T., Abbo, L., Alexandrova, O., Anastasiadis, A., Andretta, V., Antonucci, E., Appourchaux, T., Aran, A., Arge, C. N., Aulanier, G., Baker, D., Bale, S. D., Battaglia, M., Rubio, L. Bellot, Bemporad, A., Berthomier, M., Bocchialini, K., Bonnin, X., Brun, A. S., Bruno, R., Buchlin, E., Buechner, J., Bucik, R., Carcaboso, F., Carr, R., Carrasco-Blazquez, I., Cecconi, B., Cangas, I. Cernuda, Chen, C. H. K., Chitta, L. P., Chust, T., Dalmasse, K., D'Amicis, R., Da Deppo, V., De Marco, R., Dolei, S., Dolla, L., de Wit, T. Dudok, van Driel-Gesztelyi, L., Eastwood, J. P., Lara, F. Espinosa, Etesi, L., Fedorov, A., Felix-Redondo, F., Fineschi, S., Fleck, B., Fontaine, D., Fox, N. J., Gandorfer, A., Genot, V., Georgoulis, M. K., Gissot, S., Giunta, A., Gizon, L., Gomez-Herrero, R., Gontikakis, C., Graham, G., Green, L., Grundy, T., Haberreiter, M., Harra, L. K., Hassler, D. M., Hirzberger, J., Ho, G. C., Hurford, G., Innes, D., Issautier, K., James, A. W., Janitzek, N., Janvier, M., Jeffrey, N., Jenkins, J., Khotyaintsev, Y., Klein, K. -L., Kontar, E. P., Kontogiannis, I., Krafft, C., Krasnoselskikh, V., Kretzschmar, M., Labrosse, N., Lagg, A., Landini, F., Lavraud, B., Leon, I., Lepri, S. T., Lewis, G. R., Liewer, P., Linker, J., Livi, S., Long, D. M., Louarn, P., Malandraki, O., Maloney, S., Martinez-Pillet, V., Martinovic, M., Masson, A., Matthews, S., Matteini, L., Meyer-Vernet, N., Moraitis, K., Morton, R. J., Musset, S., Nicolaou, G., Nindos, A., O'Brien, H., Suarez, D. Orozco, Owens, M., Pancrazzi, M., Papaioannou, A., Parenti, S., Pariat, E., Patsourakos, S., Perrone, D., Peter, H., Pinto, R. F., Plainaki, C., Plettemeier, D., Plunkett, S. P., Raines, J. M., Raouafi, N., Reid, H., Retino, A., Rezeau, L., Rochus, P., Rodriguez, L., Rodriguez-Garcia, L., Roth, M., Rouillard, A. P., Sahraoui, F., Sasso, C., Schou, J., Schuehle, U., Sorriso-Valvo, L., Soucek, J., Spadaro, D., Stangalini, M., Stansby, D., Steller, M., Strugarek, A., Stverak, S., Susino, R., Telloni, D., Terasa, C., Teriaca, L., Toledo-Redondo, S., Iniesta, J. C. del Toro, Tsiropoula, G., Tsounis, A., Tziotziou, K., Valentini, F., Vaivads, A., Vecchio, A., Velli, M., Verbeeck, C., Verdini, A., Verscharen, D., Vilmer, N., Vourlidas, A., Wicks, R., Wimmer-Schweingruber, R. F., Wiegelmann, T., Young, P. R., Zhukov, A. N., Zouganelis, I., De Groof, A., Walsh, A. P., Williams, D. R., Mueller, D., Cyr, O. C. St, Auchere, F., Berghmans, D., Fludra, A., Horbury, T. S., Howard, R. A., Krucker, S., Maksimovic, M., Owen, C. J., Rodriiguez-Pacheco, J., Romoli, M., Solanki, S. K., Watson, C., Sanchez, L., Lefort, J., Osuna, P., Gilbert, H. R., Nieves-Chinchilla, T., Abbo, L., Alexandrova, O., Anastasiadis, A., Andretta, V., Antonucci, E., Appourchaux, T., Aran, A., Arge, C. N., Aulanier, G., Baker, D., Bale, S. D., Battaglia, M., Rubio, L. Bellot, Bemporad, A., Berthomier, M., Bocchialini, K., Bonnin, X., Brun, A. S., Bruno, R., Buchlin, E., Buechner, J., Bucik, R., Carcaboso, F., Carr, R., Carrasco-Blazquez, I., Cecconi, B., Cangas, I. Cernuda, Chen, C. H. K., Chitta, L. P., Chust, T., Dalmasse, K., D'Amicis, R., Da Deppo, V., De Marco, R., Dolei, S., Dolla, L., de Wit, T. Dudok, van Driel-Gesztelyi, L., Eastwood, J. P., Lara, F. Espinosa, Etesi, L., Fedorov, A., Felix-Redondo, F., Fineschi, S., Fleck, B., Fontaine, D., Fox, N. J., Gandorfer, A., Genot, V., Georgoulis, M. K., Gissot, S., Giunta, A., Gizon, L., Gomez-Herrero, R., Gontikakis, C., Graham, G., Green, L., Grundy, T., Haberreiter, M., Harra, L. K., Hassler, D. M., Hirzberger, J., Ho, G. C., Hurford, G., Innes, D., Issautier, K., James, A. W., Janitzek, N., Janvier, M., Jeffrey, N., Jenkins, J., Khotyaintsev, Y., Klein, K. -L., Kontar, E. P., Kontogiannis, I., Krafft, C., Krasnoselskikh, V., Kretzschmar, M., Labrosse, N., Lagg, A., Landini, F., Lavraud, B., Leon, I., Lepri, S. T., Lewis, G. R., Liewer, P., Linker, J., Livi, S., Long, D. M., Louarn, P., Malandraki, O., Maloney, S., Martinez-Pillet, V., Martinovic, M., Masson, A., Matthews, S., Matteini, L., Meyer-Vernet, N., Moraitis, K., Morton, R. J., Musset, S., Nicolaou, G., Nindos, A., O'Brien, H., Suarez, D. Orozco, Owens, M., Pancrazzi, M., Papaioannou, A., Parenti, S., Pariat, E., Patsourakos, S., Perrone, D., Peter, H., Pinto, R. F., Plainaki, C., Plettemeier, D., Plunkett, S. P., Raines, J. M., Raouafi, N., Reid, H., Retino, A., Rezeau, L., Rochus, P., Rodriguez, L., Rodriguez-Garcia, L., Roth, M., Rouillard, A. P., Sahraoui, F., Sasso, C., Schou, J., Schuehle, U., Sorriso-Valvo, L., Soucek, J., Spadaro, D., Stangalini, M., Stansby, D., Steller, M., Strugarek, A., Stverak, S., Susino, R., Telloni, D., Terasa, C., Teriaca, L., Toledo-Redondo, S., Iniesta, J. C. del Toro, Tsiropoula, G., Tsounis, A., Tziotziou, K., Valentini, F., Vaivads, A., Vecchio, A., Velli, M., Verbeeck, C., Verdini, A., Verscharen, D., Vilmer, N., Vourlidas, A., Wicks, R., Wimmer-Schweingruber, R. F., Wiegelmann, T., Young, P. R., and Zhukov, A. N.

Abstract

Solar Orbiter is the first space mission observing the solar plasma both in situ and remotely, from a close distance, in and out of the ecliptic. The ultimate goal is to understand how the Sun produces and controls the heliosphere, filling the Solar System and driving the planetary environments. With six remote-sensing and four in-situ instrument suites, the coordination and planning of the operations are essential to address the following four top-level science questions: (1) What drives the solar wind and where does the coronal magnetic field originate? (2) How do solar transients drive heliospheric variability? (3) How do solar eruptions produce energetic particle radiation that fills the heliosphere? (4) How does the solar dynamo work and drive connections between the Sun and the heliosphere? Maximising the mission's science return requires considering the characteristics of each orbit, including the relative position of the spacecraft to Earth (affecting downlink rates), trajectory events (such as gravitational assist manoeuvres), and the phase of the solar activity cycle. Furthermore, since each orbit's science telemetry will be downloaded over the course of the following orbit, science operations must be planned at mission level, rather than at the level of individual orbits. It is important to explore the way in which those science questions are translated into an actual plan of observations that fits into the mission, thus ensuring that no opportunities are missed. First, the overarching goals are broken down into specific, answerable questions along with the required observations and the so-called Science Activity Plan (SAP) is developed to achieve this. The SAP groups objectives that require similar observations into Solar Orbiter Observing Plans (SOOPs), resulting in a strategic, top-level view of the optimal opportunities for science observations during the mission lifetime., Comment: 20 pages, 1 figure, accepted by Astronomy & Astrophysics

Published
2020
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7. The Solar Orbiter mission -- Science overview

Author

Müller, D., Cyr, O. C. St., Zouganelis, I., Gilbert, H. R., Marsden, R., Nieves-Chinchilla, T., Antonucci, E., Auchère, F., Berghmans, D., Horbury, T., Howard, R. A., Krucker, S., Maksimovic, M., Owen, C. J., Rochus, P., Rodriguez-Pacheco, J., Romoli, M., Solanki, S. K., Bruno, R., Carlsson, M., Fludra, A., Harra, L., Hassler, D. M., Livi, S., Louarn, P., Peter, H., Schühle, U., Teriaca, L., Iniesta, J. C. del Toro, Wimmer-Schweingruber, R. F., Marsch, E., Velli, M., De Groof, A., Walsh, A., Williams, D., Müller, D., Cyr, O. C. St., Zouganelis, I., Gilbert, H. R., Marsden, R., Nieves-Chinchilla, T., Antonucci, E., Auchère, F., Berghmans, D., Horbury, T., Howard, R. A., Krucker, S., Maksimovic, M., Owen, C. J., Rochus, P., Rodriguez-Pacheco, J., Romoli, M., Solanki, S. K., Bruno, R., Carlsson, M., Fludra, A., Harra, L., Hassler, D. M., Livi, S., Louarn, P., Peter, H., Schühle, U., Teriaca, L., Iniesta, J. C. del Toro, Wimmer-Schweingruber, R. F., Marsch, E., Velli, M., De Groof, A., Walsh, A., and Williams, D.

Abstract

Solar Orbiter, the first mission of ESA's Cosmic Vision 2015-2025 programme and a mission of international collaboration between ESA and NASA, will explore the Sun and heliosphere from close up and out of the ecliptic plane. It was launched on 10 February 2020 04:03 UTC from Cape Canaveral and aims to address key questions of solar and heliospheric physics pertaining to how the Sun creates and controls the Heliosphere, and why solar activity changes with time. To answer these, the mission carries six remote-sensing instruments to observe the Sun and the solar corona, and four in-situ instruments to measure the solar wind, energetic particles, and electromagnetic fields. In this paper, we describe the science objectives of the mission, and how these will be addressed by the joint observations of the instruments onboard. The paper first summarises the mission-level science objectives, followed by an overview of the spacecraft and payload. We report the observables and performance figures of each instrument, as well as the trajectory design. This is followed by a summary of the science operations concept. The paper concludes with a more detailed description of the science objectives. Solar Orbiter will combine in-situ measurements in the heliosphere with high-resolution remote-sensing observations of the Sun to address fundamental questions of solar and heliospheric physics. The performance of the Solar Orbiter payload meets the requirements derived from the mission's science objectives. Its science return will be augmented further by coordinated observations with other space missions and ground-based observatories., Comment: 32 pages, 30 figures; accepted for publication in A&A

Published
2020
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8. The Solar Orbiter mission: Science overview

Author

German Centre for Air and Space Travel, Max Planck Society, Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Centre National D'Etudes Spatiales (France), Müller, D., St. Cyr, O. C., Zouganelis, I., Gilbert, H. R., Marsden, R., Nieves-Chinchilla, T., Antonucci, E., Auchère, Frederic, Berghmans, D., Horbury, T. S., Howard, R. A., Krucker, S., Maksimovic, M., Owen, C. J., Rochus, P., Rodriguez-Pacheco, J., Romoli, M., Solanki, S. K., Bruno, R., Carlsson, M., Fludra, A., Harra, L., Hassler, D. M., Livi, S., Louarn, P., Peter, H., Schühle, U., Teriaca, L., Toro, José Carlos del, Wimmer-Schweingruber, R. F., Marsch, E., Velli, M., De Groof, A., Walsh, Andrew J., Williams, D., German Centre for Air and Space Travel, Max Planck Society, Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Centre National D'Etudes Spatiales (France), Müller, D., St. Cyr, O. C., Zouganelis, I., Gilbert, H. R., Marsden, R., Nieves-Chinchilla, T., Antonucci, E., Auchère, Frederic, Berghmans, D., Horbury, T. S., Howard, R. A., Krucker, S., Maksimovic, M., Owen, C. J., Rochus, P., Rodriguez-Pacheco, J., Romoli, M., Solanki, S. K., Bruno, R., Carlsson, M., Fludra, A., Harra, L., Hassler, D. M., Livi, S., Louarn, P., Peter, H., Schühle, U., Teriaca, L., Toro, José Carlos del, Wimmer-Schweingruber, R. F., Marsch, E., Velli, M., De Groof, A., Walsh, Andrew J., and Williams, D.

Abstract

Aims. Solar Orbiter, the first mission of ESA's Cosmic Vision 2015-2025 programme and a mission of international collaboration between ESA and NASA, will explore the Sun and heliosphere from close up and out of the ecliptic plane. It was launched on 10 February 2020 04:03 UTC from Cape Canaveral and aims to address key questions of solar and heliospheric physics pertaining to how the Sun creates and controls the Heliosphere, and why solar activity changes with time. To answer these, the mission carries six remote-sensing instruments to observe the Sun and the solar corona, and four in-situ instruments to measure the solar wind, energetic particles, and electromagnetic fields. In this paper, we describe the science objectives of the mission, and how these will be addressed by the joint observations of the instruments onboard. Methods. The paper first summarises the mission-level science objectives, followed by an overview of the spacecraft and payload. We report the observables and performance figures of each instrument, as well as the trajectory design. This is followed by a summary of the science operations concept. The paper concludes with a more detailed description of the science objectives. Results. Solar Orbiter will combine in-situ measurements in the heliosphere with high-resolution remote-sensing observations of the Sun to address fundamental questions of solar and heliospheric physics. The performance of the Solar Orbiter payload meets the requirements derived from the mission's science objectives. Its science return will be augmented further by coordinated observations with other space missions and ground-based observatories. © 2020 ESO.

Published
2020

9. The Solar Orbiter SPICE instrument -- An extreme UV imaging spectrometer

Author

Consortium, The SPICE, Anderson, M., Appourchaux, T., Auchère, F., Cuadrado, R. Aznar, Barbay, J., Baudin, F., Beardsley, S., Bocchialini, K., Borgo, B., Bruzzi, D., Buchlin, E., Burton, G., Blüchel, V., Caldwell, M., Caminade, S., Carlsson, M., Curdt, W., Davenne, J., Davila, J., DeForest, C. E., Del Zanna, G., Drummond, D., Dubau, J., Dumesnil, C., Dunn, G., Eccleston, P., Fludra, A., Fredvik, T., Gabriel, A., Giunta, A., Gottwald, A., Griffin, D., Grundy, T., Guest, S., Gyo, M., Haberreiter, M., Hansteen, V., Harrison, R., Hassler, D. M., Haugan, S. V. H., Howe, C., Janvier, M., Klein, R., Koller, S., Kucera, T. A., Kouliche, D., Marsch, E., Marshall, A., Marshall, G., Matthews, S. A., McQuirk, C., Meining, S., Mercier, C., Morris, N., Morse, T., Munro, G., Parenti, S., Pastor-Santos, C., Peter, H., Pfiffner, D., Phelan, P., Philippon, A., Richards, A., Rogers, K., Sawyer, C., Schlatter, P., Schmutz, W., Schühle, U., Shaughnessy, B., Sidher, S., Solanki, S. K., Speight, R., Spescha, M., Szwec, N., Tamiatto, C., Teriaca, L., Thompson, W., Tosh, I., Tustain, S., Vial, J. -C., Walls, B., Waltham, N., Wimmer-Schweingruber, R., Woodward, S., Young, P., De Groof, A., Pacros, A., Williams, D., Müller, D., Consortium, The SPICE, Anderson, M., Appourchaux, T., Auchère, F., Cuadrado, R. Aznar, Barbay, J., Baudin, F., Beardsley, S., Bocchialini, K., Borgo, B., Bruzzi, D., Buchlin, E., Burton, G., Blüchel, V., Caldwell, M., Caminade, S., Carlsson, M., Curdt, W., Davenne, J., Davila, J., DeForest, C. E., Del Zanna, G., Drummond, D., Dubau, J., Dumesnil, C., Dunn, G., Eccleston, P., Fludra, A., Fredvik, T., Gabriel, A., Giunta, A., Gottwald, A., Griffin, D., Grundy, T., Guest, S., Gyo, M., Haberreiter, M., Hansteen, V., Harrison, R., Hassler, D. M., Haugan, S. V. H., Howe, C., Janvier, M., Klein, R., Koller, S., Kucera, T. A., Kouliche, D., Marsch, E., Marshall, A., Marshall, G., Matthews, S. A., McQuirk, C., Meining, S., Mercier, C., Morris, N., Morse, T., Munro, G., Parenti, S., Pastor-Santos, C., Peter, H., Pfiffner, D., Phelan, P., Philippon, A., Richards, A., Rogers, K., Sawyer, C., Schlatter, P., Schmutz, W., Schühle, U., Shaughnessy, B., Sidher, S., Solanki, S. K., Speight, R., Spescha, M., Szwec, N., Tamiatto, C., Teriaca, L., Thompson, W., Tosh, I., Tustain, S., Vial, J. -C., Walls, B., Waltham, N., Wimmer-Schweingruber, R., Woodward, S., Young, P., De Groof, A., Pacros, A., Williams, D., and Müller, D.

Abstract

The Spectral Imaging of the Coronal Environment (SPICE) instrument is a high-resolution imaging spectrometer operating at extreme ultraviolet (EUV) wavelengths. In this paper, we present the concept, design, and pre-launch performance of this facility instrument on the ESA/NASA Solar Orbiter mission. The goal of this paper is to give prospective users a better understanding of the possible types of observations, the data acquisition, and the sources that contribute to the instrument's signal. The paper discusses the science objectives, with a focus on the SPICE-specific aspects, before presenting the instrument's design, including optical, mechanical, thermal, and electronics aspects. This is followed by a characterisation and calibration of the instrument's performance. The paper concludes with descriptions of the operations concept and data processing. The performance measurements of the various instrument parameters meet the requirements derived from the mission's science objectives. The SPICE instrument is ready to perform measurements that will provide vital contributions to the scientific success of the Solar Orbiter mission., Comment: A&A, accepted 19 August 2019; 26 pages, 25 figures

Published
2019
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10. The Solar Orbiter SPICE instrument -- An extreme UV imaging spectrometer

Author

Consortium, The SPICE, Anderson, M., Appourchaux, T., Auchère, F., Cuadrado, R. Aznar, Barbay, J., Baudin, F., Beardsley, S., Bocchialini, K., Borgo, B., Bruzzi, D., Buchlin, E., Burton, G., Blüchel, V., Caldwell, M., Caminade, S., Carlsson, M., Curdt, W., Davenne, J., Davila, J., DeForest, C. E., Del Zanna, G., Drummond, D., Dubau, J., Dumesnil, C., Dunn, G., Eccleston, P., Fludra, A., Fredvik, T., Gabriel, A., Giunta, A., Gottwald, A., Griffin, D., Grundy, T., Guest, S., Gyo, M., Haberreiter, M., Hansteen, V., Harrison, R., Hassler, D. M., Haugan, S. V. H., Howe, C., Janvier, M., Klein, R., Koller, S., Kucera, T. A., Kouliche, D., Marsch, E., Marshall, A., Marshall, G., Matthews, S. A., McQuirk, C., Meining, S., Mercier, C., Morris, N., Morse, T., Munro, G., Parenti, S., Pastor-Santos, C., Peter, H., Pfiffner, D., Phelan, P., Philippon, A., Richards, A., Rogers, K., Sawyer, C., Schlatter, P., Schmutz, W., Schühle, U., Shaughnessy, B., Sidher, S., Solanki, S. K., Speight, R., Spescha, M., Szwec, N., Tamiatto, C., Teriaca, L., Thompson, W., Tosh, I., Tustain, S., Vial, J. -C., Walls, B., Waltham, N., Wimmer-Schweingruber, R., Woodward, S., Young, P., De Groof, A., Pacros, A., Williams, D., Müller, D., Consortium, The SPICE, Anderson, M., Appourchaux, T., Auchère, F., Cuadrado, R. Aznar, Barbay, J., Baudin, F., Beardsley, S., Bocchialini, K., Borgo, B., Bruzzi, D., Buchlin, E., Burton, G., Blüchel, V., Caldwell, M., Caminade, S., Carlsson, M., Curdt, W., Davenne, J., Davila, J., DeForest, C. E., Del Zanna, G., Drummond, D., Dubau, J., Dumesnil, C., Dunn, G., Eccleston, P., Fludra, A., Fredvik, T., Gabriel, A., Giunta, A., Gottwald, A., Griffin, D., Grundy, T., Guest, S., Gyo, M., Haberreiter, M., Hansteen, V., Harrison, R., Hassler, D. M., Haugan, S. V. H., Howe, C., Janvier, M., Klein, R., Koller, S., Kucera, T. A., Kouliche, D., Marsch, E., Marshall, A., Marshall, G., Matthews, S. A., McQuirk, C., Meining, S., Mercier, C., Morris, N., Morse, T., Munro, G., Parenti, S., Pastor-Santos, C., Peter, H., Pfiffner, D., Phelan, P., Philippon, A., Richards, A., Rogers, K., Sawyer, C., Schlatter, P., Schmutz, W., Schühle, U., Shaughnessy, B., Sidher, S., Solanki, S. K., Speight, R., Spescha, M., Szwec, N., Tamiatto, C., Teriaca, L., Thompson, W., Tosh, I., Tustain, S., Vial, J. -C., Walls, B., Waltham, N., Wimmer-Schweingruber, R., Woodward, S., Young, P., De Groof, A., Pacros, A., Williams, D., and Müller, D.

Abstract

The Spectral Imaging of the Coronal Environment (SPICE) instrument is a high-resolution imaging spectrometer operating at extreme ultraviolet (EUV) wavelengths. In this paper, we present the concept, design, and pre-launch performance of this facility instrument on the ESA/NASA Solar Orbiter mission. The goal of this paper is to give prospective users a better understanding of the possible types of observations, the data acquisition, and the sources that contribute to the instrument's signal. The paper discusses the science objectives, with a focus on the SPICE-specific aspects, before presenting the instrument's design, including optical, mechanical, thermal, and electronics aspects. This is followed by a characterisation and calibration of the instrument's performance. The paper concludes with descriptions of the operations concept and data processing. The performance measurements of the various instrument parameters meet the requirements derived from the mission's science objectives. The SPICE instrument is ready to perform measurements that will provide vital contributions to the scientific success of the Solar Orbiter mission., Comment: A&A, accepted 19 August 2019; 26 pages, 25 figures

Published
2019
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11. Interplanetary coronal mass ejection observed at STEREO-A, Mars, comet 67P/Churyumov-Gerasimenko, Saturn, and New Horizons en route to Pluto : Comparison of its Forbush decreases at 1.4, 3.1, and 9.9 AU

Author

Witasse, O., Sanchez-Cano, B., Mays, M. L., Kajdic, P., Opgenoorth, Hermann, Elliott, H. A., Richardson, I. G., Zouganelis, I., Zender, J., Wimmer-Schweingruber, R. F., Turc, L., Taylor, M. G. G. T., Roussos, E., Rouillard, A., Richter, I., Richardson, J. D., Ramstad, R., Provan, G., Posner, A., Plaut, J. J., Odstrcil, D., Nilsson, H., Niemenen, P., Milan, S. E., Mandt, K., Lohf, H., Lester, M., Lebreton, J. -P, Kuulkers, E., Krupp, N., Koenders, C., James, M. K., Intzekara, D., Holmstrom, M., Hassler, D. M., Hall, B. E. S., Guo, J., Goldstein, R., Goetz, C., Glassmeier, K. H., Genot, V., Evans, H., Espley, J., Edberg, N. J. T., Edberg, Niklas J. T., Cowley, S. W. H., Burch, J., Behar, E., Barabash, S., Andrews, David J., Altobelli, N., Witasse, O., Sanchez-Cano, B., Mays, M. L., Kajdic, P., Opgenoorth, Hermann, Elliott, H. A., Richardson, I. G., Zouganelis, I., Zender, J., Wimmer-Schweingruber, R. F., Turc, L., Taylor, M. G. G. T., Roussos, E., Rouillard, A., Richter, I., Richardson, J. D., Ramstad, R., Provan, G., Posner, A., Plaut, J. J., Odstrcil, D., Nilsson, H., Niemenen, P., Milan, S. E., Mandt, K., Lohf, H., Lester, M., Lebreton, J. -P, Kuulkers, E., Krupp, N., Koenders, C., James, M. K., Intzekara, D., Holmstrom, M., Hassler, D. M., Hall, B. E. S., Guo, J., Goldstein, R., Goetz, C., Glassmeier, K. H., Genot, V., Evans, H., Espley, J., Edberg, N. J. T., Edberg, Niklas J. T., Cowley, S. W. H., Burch, J., Behar, E., Barabash, S., Andrews, David J., and Altobelli, N.

Abstract

We discuss observations of the journey throughout the Solar System of a large interplanetary coronal mass ejection (ICME) that was ejected at the Sun on 14 October 2014. The ICME hit Mars on 17 October, as observed by the Mars Express, Mars Atmosphere and Volatile EvolutioN Mission (MAVEN), Mars Odyssey, and Mars Science Laboratory (MSL) missions, 44h before the encounter of the planet with the Siding-Spring comet, for which the space weather context is provided. It reached comet 67P/Churyumov-Gerasimenko, which was perfectly aligned with the Sun and Mars at 3.1 AU, as observed by Rosetta on 22 October. The ICME was also detected by STEREO-A on 16 October at 1 AU, and by Cassini in the solar wind around Saturn on the 12 November at 9.9AU. Fortuitously, the New Horizons spacecraft was also aligned with the direction of the ICME at 31.6 AU. We investigate whether this ICME has a nonambiguous signature at New Horizons. A potential detection of this ICME by Voyager 2 at 110-111 AU is also discussed. The multispacecraft observations allow the derivation of certain properties of the ICME, such as its large angular extension of at least 116 degrees, its speed as a function of distance, and its magnetic field structure at four locations from 1 to 10 AU. Observations of the speed data allow two different solar wind propagation models to be validated. Finally, we compare the Forbush decreases (transient decreases followed by gradual recoveries in the galactic cosmic ray intensity) due to the passage of this ICME at Mars, comet 67P, and Saturn.

Published
2017
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12. Interplanetary coronal mass ejection observed at STEREO-A, Mars, comet 67P/Churyumov-Gerasimenko, Saturn, and New Horizons en route to Pluto : Comparison of its Forbush decreases at 1.4, 3.1, and 9.9 AU

Author

Witasse, O., Sanchez-Cano, B., Mays, M. L., Kajdic, P., Opgenoorth, Hermann, Elliott, H. A., Richardson, I. G., Zouganelis, I., Zender, J., Wimmer-Schweingruber, R. F., Turc, L., Taylor, M. G. G. T., Roussos, E., Rouillard, A., Richter, I., Richardson, J. D., Ramstad, R., Provan, G., Posner, A., Plaut, J. J., Odstrcil, D., Nilsson, H., Niemenen, P., Milan, S. E., Mandt, K., Lohf, H., Lester, M., Lebreton, J. -P, Kuulkers, E., Krupp, N., Koenders, C., James, M. K., Intzekara, D., Holmstrom, M., Hassler, D. M., Hall, B. E. S., Guo, J., Goldstein, R., Goetz, C., Glassmeier, K. H., Genot, V., Evans, H., Espley, J., Edberg, N. J. T., Edberg, Niklas J. T., Cowley, S. W. H., Burch, J., Behar, E., Barabash, S., Andrews, David J., Altobelli, N., Witasse, O., Sanchez-Cano, B., Mays, M. L., Kajdic, P., Opgenoorth, Hermann, Elliott, H. A., Richardson, I. G., Zouganelis, I., Zender, J., Wimmer-Schweingruber, R. F., Turc, L., Taylor, M. G. G. T., Roussos, E., Rouillard, A., Richter, I., Richardson, J. D., Ramstad, R., Provan, G., Posner, A., Plaut, J. J., Odstrcil, D., Nilsson, H., Niemenen, P., Milan, S. E., Mandt, K., Lohf, H., Lester, M., Lebreton, J. -P, Kuulkers, E., Krupp, N., Koenders, C., James, M. K., Intzekara, D., Holmstrom, M., Hassler, D. M., Hall, B. E. S., Guo, J., Goldstein, R., Goetz, C., Glassmeier, K. H., Genot, V., Evans, H., Espley, J., Edberg, N. J. T., Edberg, Niklas J. T., Cowley, S. W. H., Burch, J., Behar, E., Barabash, S., Andrews, David J., and Altobelli, N.

Abstract

We discuss observations of the journey throughout the Solar System of a large interplanetary coronal mass ejection (ICME) that was ejected at the Sun on 14 October 2014. The ICME hit Mars on 17 October, as observed by the Mars Express, Mars Atmosphere and Volatile EvolutioN Mission (MAVEN), Mars Odyssey, and Mars Science Laboratory (MSL) missions, 44h before the encounter of the planet with the Siding-Spring comet, for which the space weather context is provided. It reached comet 67P/Churyumov-Gerasimenko, which was perfectly aligned with the Sun and Mars at 3.1 AU, as observed by Rosetta on 22 October. The ICME was also detected by STEREO-A on 16 October at 1 AU, and by Cassini in the solar wind around Saturn on the 12 November at 9.9AU. Fortuitously, the New Horizons spacecraft was also aligned with the direction of the ICME at 31.6 AU. We investigate whether this ICME has a nonambiguous signature at New Horizons. A potential detection of this ICME by Voyager 2 at 110-111 AU is also discussed. The multispacecraft observations allow the derivation of certain properties of the ICME, such as its large angular extension of at least 116 degrees, its speed as a function of distance, and its magnetic field structure at four locations from 1 to 10 AU. Observations of the speed data allow two different solar wind propagation models to be validated. Finally, we compare the Forbush decreases (transient decreases followed by gradual recoveries in the galactic cosmic ray intensity) due to the passage of this ICME at Mars, comet 67P, and Saturn.

Published
2017
Full Text
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13. Interplanetary coronal mass ejection observed at STEREO-A, Mars, comet 67P/Churyumov-Gerasimenko, Saturn, and New Horizons en route to Pluto : Comparison of its Forbush decreases at 1.4, 3.1, and 9.9 AU

Author

Witasse, O., Sanchez-Cano, B., Mays, M. L., Kajdic, P., Opgenoorth, Hermann, Elliott, H. A., Richardson, I. G., Zouganelis, I., Zender, J., Wimmer-Schweingruber, R. F., Turc, L., Taylor, M. G. G. T., Roussos, E., Rouillard, A., Richter, I., Richardson, J. D., Ramstad, R., Provan, G., Posner, A., Plaut, J. J., Odstrcil, D., Nilsson, H., Niemenen, P., Milan, S. E., Mandt, K., Lohf, H., Lester, M., Lebreton, J. -P, Kuulkers, E., Krupp, N., Koenders, C., James, M. K., Intzekara, D., Holmstrom, M., Hassler, D. M., Hall, B. E. S., Guo, J., Goldstein, R., Goetz, C., Glassmeier, K. H., Genot, V., Evans, H., Espley, J., Edberg, N. J. T., Edberg, Niklas J. T., Cowley, S. W. H., Burch, J., Behar, E., Barabash, S., Andrews, David J., Altobelli, N., Witasse, O., Sanchez-Cano, B., Mays, M. L., Kajdic, P., Opgenoorth, Hermann, Elliott, H. A., Richardson, I. G., Zouganelis, I., Zender, J., Wimmer-Schweingruber, R. F., Turc, L., Taylor, M. G. G. T., Roussos, E., Rouillard, A., Richter, I., Richardson, J. D., Ramstad, R., Provan, G., Posner, A., Plaut, J. J., Odstrcil, D., Nilsson, H., Niemenen, P., Milan, S. E., Mandt, K., Lohf, H., Lester, M., Lebreton, J. -P, Kuulkers, E., Krupp, N., Koenders, C., James, M. K., Intzekara, D., Holmstrom, M., Hassler, D. M., Hall, B. E. S., Guo, J., Goldstein, R., Goetz, C., Glassmeier, K. H., Genot, V., Evans, H., Espley, J., Edberg, N. J. T., Edberg, Niklas J. T., Cowley, S. W. H., Burch, J., Behar, E., Barabash, S., Andrews, David J., and Altobelli, N.

Abstract

We discuss observations of the journey throughout the Solar System of a large interplanetary coronal mass ejection (ICME) that was ejected at the Sun on 14 October 2014. The ICME hit Mars on 17 October, as observed by the Mars Express, Mars Atmosphere and Volatile EvolutioN Mission (MAVEN), Mars Odyssey, and Mars Science Laboratory (MSL) missions, 44h before the encounter of the planet with the Siding-Spring comet, for which the space weather context is provided. It reached comet 67P/Churyumov-Gerasimenko, which was perfectly aligned with the Sun and Mars at 3.1 AU, as observed by Rosetta on 22 October. The ICME was also detected by STEREO-A on 16 October at 1 AU, and by Cassini in the solar wind around Saturn on the 12 November at 9.9AU. Fortuitously, the New Horizons spacecraft was also aligned with the direction of the ICME at 31.6 AU. We investigate whether this ICME has a nonambiguous signature at New Horizons. A potential detection of this ICME by Voyager 2 at 110-111 AU is also discussed. The multispacecraft observations allow the derivation of certain properties of the ICME, such as its large angular extension of at least 116 degrees, its speed as a function of distance, and its magnetic field structure at four locations from 1 to 10 AU. Observations of the speed data allow two different solar wind propagation models to be validated. Finally, we compare the Forbush decreases (transient decreases followed by gradual recoveries in the galactic cosmic ray intensity) due to the passage of this ICME at Mars, comet 67P, and Saturn.

Published
2017
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14. Interplanetary coronal mass ejection observed at STEREO-A, Mars, comet 67P/Churyumov-Gerasimenko, Saturn, and New Horizons en-route to Pluto. Comparison of its Forbush decreases at 1.4, 3.1 and 9.9 AU:Interplanetary coronal mass ejection

Author

Witasse, Olivier, Sánchez-Cano, Beatriz, Mays, M. L., Kajdič, P., Opgenoorth, Hermann, Elliott, H. A., Richardson, I. G., Zouganelis, I., Zender, J., Wimmer-Schweingruber, R. F., Turc, L., Taylor, M. G. G. T., Roussos, E., Rouillard, A., Richter, I., Richardson, J. D., Ramstad, R., Provan, G., Posner, A., Plaut, J. J., Odstrcil, D., Nilsson, H., Niemenen, P., Milan, S. E., Mandt, K., Lohf, H., Lester, Mark, Lebreton, J.-P., Kuulkers, E., Krupp, N., Koenders, C., James, M. K., Intzekara, D., Holmstrom, Mats, Hassler, D. M., Hall, B. E. S., Guo, J., Goldstein, R., Goetz, C., Glassmeier, K. H., Génot, V., Evans, H., Espley, J., Edberg, Niklas, Dougherty, M., Cowley, S. W. H., Burch, J., Behar, E., Barabash, Stas, Andrews, David, Altobelli, N., Witasse, Olivier, Sánchez-Cano, Beatriz, Mays, M. L., Kajdič, P., Opgenoorth, Hermann, Elliott, H. A., Richardson, I. G., Zouganelis, I., Zender, J., Wimmer-Schweingruber, R. F., Turc, L., Taylor, M. G. G. T., Roussos, E., Rouillard, A., Richter, I., Richardson, J. D., Ramstad, R., Provan, G., Posner, A., Plaut, J. J., Odstrcil, D., Nilsson, H., Niemenen, P., Milan, S. E., Mandt, K., Lohf, H., Lester, Mark, Lebreton, J.-P., Kuulkers, E., Krupp, N., Koenders, C., James, M. K., Intzekara, D., Holmstrom, Mats, Hassler, D. M., Hall, B. E. S., Guo, J., Goldstein, R., Goetz, C., Glassmeier, K. H., Génot, V., Evans, H., Espley, J., Edberg, Niklas, Dougherty, M., Cowley, S. W. H., Burch, J., Behar, E., Barabash, Stas, Andrews, David, and Altobelli, N.

Abstract

We discuss observations of the journey throughout the Solar System of a large interplanetary coronal mass ejection (ICME) that was ejected at the Sun on 14 October 2014. The ICME hit Mars on 17 October, as observed by the Mars Express, MAVEN, Mars Odyssey and MSL missions, 44 hours before the encounter of the planet with the Siding-Spring comet, for which the space weather context is provided. It reached comet 67P/Churyumov-Gerasimenko, which was perfectly aligned with the Sun and Mars at 3.1 AU, as observed by Rosetta on 22 October. The ICME was also detected by STEREO-A on 16 October at 1 AU, and by Cassini in the solar wind around Saturn on the 12 November at 9.9 AU. Fortuitously, the New Horizons spacecraft was also aligned with the direction of the ICME at 31.6 AU. We investigate whether this ICME has a non-ambiguous signature at New Horizons. A potential detection of this ICME by Voyager-2 at 110-111 AU is also discussed. The multi-spacecraft observations allow the derivation of certain properties of the ICME, such as its large angular extension of at least 116°, its speed as a function of distance, and its magnetic field structure at four locations from 1 to 10 AU. Observations of the speed data allow two different solar wind propagation models to be validated. Finally, we compare the Forbush decreases (transient decreases followed by gradual recoveries in the galactic cosmic ray intensity) due to the passage of this ICME at Mars, comet 67P and Saturn.

Published
2017

15. Interplanetary coronal mass ejection observed at STEREO-A, Mars, comet 67P/Churyumov-Gerasimenko, Saturn, and New Horizons en route to Pluto : Comparison of its Forbush decreases at 1.4, 3.1, and 9.9 AU

Author

Witasse, O., Sanchez-Cano, B., Mays, M. L., Kajdic, P., Opgenoorth, Hermann, Elliott, H. A., Richardson, I. G., Zouganelis, I., Zender, J., Wimmer-Schweingruber, R. F., Turc, L., Taylor, M. G. G. T., Roussos, E., Rouillard, A., Richter, I., Richardson, J. D., Ramstad, R., Provan, G., Posner, A., Plaut, J. J., Odstrcil, D., Nilsson, H., Niemenen, P., Milan, S. E., Mandt, K., Lohf, H., Lester, M., Lebreton, J. -P, Kuulkers, E., Krupp, N., Koenders, C., James, M. K., Intzekara, D., Holmstrom, M., Hassler, D. M., Hall, B. E. S., Guo, J., Goldstein, R., Goetz, C., Glassmeier, K. H., Genot, V., Evans, H., Espley, J., Edberg, N. J. T., Edberg, Niklas J. T., Cowley, S. W. H., Burch, J., Behar, E., Barabash, S., Andrews, David J., Altobelli, N., Witasse, O., Sanchez-Cano, B., Mays, M. L., Kajdic, P., Opgenoorth, Hermann, Elliott, H. A., Richardson, I. G., Zouganelis, I., Zender, J., Wimmer-Schweingruber, R. F., Turc, L., Taylor, M. G. G. T., Roussos, E., Rouillard, A., Richter, I., Richardson, J. D., Ramstad, R., Provan, G., Posner, A., Plaut, J. J., Odstrcil, D., Nilsson, H., Niemenen, P., Milan, S. E., Mandt, K., Lohf, H., Lester, M., Lebreton, J. -P, Kuulkers, E., Krupp, N., Koenders, C., James, M. K., Intzekara, D., Holmstrom, M., Hassler, D. M., Hall, B. E. S., Guo, J., Goldstein, R., Goetz, C., Glassmeier, K. H., Genot, V., Evans, H., Espley, J., Edberg, N. J. T., Edberg, Niklas J. T., Cowley, S. W. H., Burch, J., Behar, E., Barabash, S., Andrews, David J., and Altobelli, N.

Abstract

We discuss observations of the journey throughout the Solar System of a large interplanetary coronal mass ejection (ICME) that was ejected at the Sun on 14 October 2014. The ICME hit Mars on 17 October, as observed by the Mars Express, Mars Atmosphere and Volatile EvolutioN Mission (MAVEN), Mars Odyssey, and Mars Science Laboratory (MSL) missions, 44h before the encounter of the planet with the Siding-Spring comet, for which the space weather context is provided. It reached comet 67P/Churyumov-Gerasimenko, which was perfectly aligned with the Sun and Mars at 3.1 AU, as observed by Rosetta on 22 October. The ICME was also detected by STEREO-A on 16 October at 1 AU, and by Cassini in the solar wind around Saturn on the 12 November at 9.9AU. Fortuitously, the New Horizons spacecraft was also aligned with the direction of the ICME at 31.6 AU. We investigate whether this ICME has a nonambiguous signature at New Horizons. A potential detection of this ICME by Voyager 2 at 110-111 AU is also discussed. The multispacecraft observations allow the derivation of certain properties of the ICME, such as its large angular extension of at least 116 degrees, its speed as a function of distance, and its magnetic field structure at four locations from 1 to 10 AU. Observations of the speed data allow two different solar wind propagation models to be validated. Finally, we compare the Forbush decreases (transient decreases followed by gradual recoveries in the galactic cosmic ray intensity) due to the passage of this ICME at Mars, comet 67P, and Saturn.

Published
2017
Full Text
View/download PDF

16. Interplanetary coronal mass ejection observed at STEREO-A, Mars, comet 67P/Churyumov-Gerasimenko, Saturn, and New Horizons en-route to Pluto. Comparison of its Forbush decreases at 1.4, 3.1 and 9.9 AU:Interplanetary coronal mass ejection

Author

Witasse, Olivier, Sánchez-Cano, Beatriz, Mays, M. L., Kajdič, P., Opgenoorth, Hermann, Elliott, H. A., Richardson, I. G., Zouganelis, I., Zender, J., Wimmer-Schweingruber, R. F., Turc, L., Taylor, M. G. G. T., Roussos, E., Rouillard, A., Richter, I., Richardson, J. D., Ramstad, R., Provan, G., Posner, A., Plaut, J. J., Odstrcil, D., Nilsson, H., Niemenen, P., Milan, S. E., Mandt, K., Lohf, H., Lester, Mark, Lebreton, J.-P., Kuulkers, E., Krupp, N., Koenders, C., James, M. K., Intzekara, D., Holmstrom, Mats, Hassler, D. M., Hall, B. E. S., Guo, J., Goldstein, R., Goetz, C., Glassmeier, K. H., Génot, V., Evans, H., Espley, J., Edberg, Niklas, Dougherty, M., Cowley, S. W. H., Burch, J., Behar, E., Barabash, Stas, Andrews, David, Altobelli, N., Witasse, Olivier, Sánchez-Cano, Beatriz, Mays, M. L., Kajdič, P., Opgenoorth, Hermann, Elliott, H. A., Richardson, I. G., Zouganelis, I., Zender, J., Wimmer-Schweingruber, R. F., Turc, L., Taylor, M. G. G. T., Roussos, E., Rouillard, A., Richter, I., Richardson, J. D., Ramstad, R., Provan, G., Posner, A., Plaut, J. J., Odstrcil, D., Nilsson, H., Niemenen, P., Milan, S. E., Mandt, K., Lohf, H., Lester, Mark, Lebreton, J.-P., Kuulkers, E., Krupp, N., Koenders, C., James, M. K., Intzekara, D., Holmstrom, Mats, Hassler, D. M., Hall, B. E. S., Guo, J., Goldstein, R., Goetz, C., Glassmeier, K. H., Génot, V., Evans, H., Espley, J., Edberg, Niklas, Dougherty, M., Cowley, S. W. H., Burch, J., Behar, E., Barabash, Stas, Andrews, David, and Altobelli, N.

Abstract

We discuss observations of the journey throughout the Solar System of a large interplanetary coronal mass ejection (ICME) that was ejected at the Sun on 14 October 2014. The ICME hit Mars on 17 October, as observed by the Mars Express, MAVEN, Mars Odyssey and MSL missions, 44 hours before the encounter of the planet with the Siding-Spring comet, for which the space weather context is provided. It reached comet 67P/Churyumov-Gerasimenko, which was perfectly aligned with the Sun and Mars at 3.1 AU, as observed by Rosetta on 22 October. The ICME was also detected by STEREO-A on 16 October at 1 AU, and by Cassini in the solar wind around Saturn on the 12 November at 9.9 AU. Fortuitously, the New Horizons spacecraft was also aligned with the direction of the ICME at 31.6 AU. We investigate whether this ICME has a non-ambiguous signature at New Horizons. A potential detection of this ICME by Voyager-2 at 110-111 AU is also discussed. The multi-spacecraft observations allow the derivation of certain properties of the ICME, such as its large angular extension of at least 116°, its speed as a function of distance, and its magnetic field structure at four locations from 1 to 10 AU. Observations of the speed data allow two different solar wind propagation models to be validated. Finally, we compare the Forbush decreases (transient decreases followed by gradual recoveries in the galactic cosmic ray intensity) due to the passage of this ICME at Mars, comet 67P and Saturn.

Published
2017

17. Interplanetary coronal mass ejection observed at STEREO-A, Mars, comet 67P/Churyumov-Gerasimenko, Saturn, and New Horizons en route to Pluto : Comparison of its Forbush decreases at 1.4, 3.1, and 9.9 AU

Author

Witasse, O., Sanchez-Cano, B., Mays, M. L., Kajdic, P., Opgenoorth, Hermann, Elliott, H. A., Richardson, I. G., Zouganelis, I., Zender, J., Wimmer-Schweingruber, R. F., Turc, L., Taylor, M. G. G. T., Roussos, E., Rouillard, A., Richter, I., Richardson, J. D., Ramstad, R., Provan, G., Posner, A., Plaut, J. J., Odstrcil, D., Nilsson, H., Niemenen, P., Milan, S. E., Mandt, K., Lohf, H., Lester, M., Lebreton, J. -P, Kuulkers, E., Krupp, N., Koenders, C., James, M. K., Intzekara, D., Holmstrom, M., Hassler, D. M., Hall, B. E. S., Guo, J., Goldstein, R., Goetz, C., Glassmeier, K. H., Genot, V., Evans, H., Espley, J., Edberg, N. J. T., Edberg, Niklas J. T., Cowley, S. W. H., Burch, J., Behar, E., Barabash, S., Andrews, David J., Altobelli, N., Witasse, O., Sanchez-Cano, B., Mays, M. L., Kajdic, P., Opgenoorth, Hermann, Elliott, H. A., Richardson, I. G., Zouganelis, I., Zender, J., Wimmer-Schweingruber, R. F., Turc, L., Taylor, M. G. G. T., Roussos, E., Rouillard, A., Richter, I., Richardson, J. D., Ramstad, R., Provan, G., Posner, A., Plaut, J. J., Odstrcil, D., Nilsson, H., Niemenen, P., Milan, S. E., Mandt, K., Lohf, H., Lester, M., Lebreton, J. -P, Kuulkers, E., Krupp, N., Koenders, C., James, M. K., Intzekara, D., Holmstrom, M., Hassler, D. M., Hall, B. E. S., Guo, J., Goldstein, R., Goetz, C., Glassmeier, K. H., Genot, V., Evans, H., Espley, J., Edberg, N. J. T., Edberg, Niklas J. T., Cowley, S. W. H., Burch, J., Behar, E., Barabash, S., Andrews, David J., and Altobelli, N.

Abstract

We discuss observations of the journey throughout the Solar System of a large interplanetary coronal mass ejection (ICME) that was ejected at the Sun on 14 October 2014. The ICME hit Mars on 17 October, as observed by the Mars Express, Mars Atmosphere and Volatile EvolutioN Mission (MAVEN), Mars Odyssey, and Mars Science Laboratory (MSL) missions, 44h before the encounter of the planet with the Siding-Spring comet, for which the space weather context is provided. It reached comet 67P/Churyumov-Gerasimenko, which was perfectly aligned with the Sun and Mars at 3.1 AU, as observed by Rosetta on 22 October. The ICME was also detected by STEREO-A on 16 October at 1 AU, and by Cassini in the solar wind around Saturn on the 12 November at 9.9AU. Fortuitously, the New Horizons spacecraft was also aligned with the direction of the ICME at 31.6 AU. We investigate whether this ICME has a nonambiguous signature at New Horizons. A potential detection of this ICME by Voyager 2 at 110-111 AU is also discussed. The multispacecraft observations allow the derivation of certain properties of the ICME, such as its large angular extension of at least 116 degrees, its speed as a function of distance, and its magnetic field structure at four locations from 1 to 10 AU. Observations of the speed data allow two different solar wind propagation models to be validated. Finally, we compare the Forbush decreases (transient decreases followed by gradual recoveries in the galactic cosmic ray intensity) due to the passage of this ICME at Mars, comet 67P, and Saturn.

Published
2017
Full Text
View/download PDF

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