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1. The Space Physics Environment Data Analysis System (SPEDAS)

Author

Angelopoulos, V., Cruce, P., Drozdov, A., Grimes, E. W., Hatzigeorgiu, N., King, D. A., Larson, D., Lewis, J. W., McTiernan, J. M., Roberts, D. A., Russell, C. L., Hori, T., Kasahara, Y., Kumamoto, A., Matsuoka, A., Miyashita, Y., Miyoshi, Y., Shinohara, I., Teramoto, M., Faden, J. B., Halford, A. J., McCarthy, M., Millan, R. M., Sample, J. G., Smith, D. M., Woodger, L. A., Masson, A., Narock, A. A., Asamura, K., Chang, T. F., Chiang, C.-Y., Kazama, Y., Keika, K., Matsuda, S., Segawa, T., Seki, K., Shoji, M., Tam, S. W. Y., Umemura, N., Wang, B.-J., Wang, S.-Y., Redmon, R., Rodriguez, J. V., Singer, H. J., Vandegriff, J., Abe, S., Nose, M., Shinbori, A., Tanaka, Y.-M., UeNo, S., Andersson, L., Dunn, P., Fowler, C., Halekas, J. S., Hara, T., Harada, Y., Lee, C. O., Lillis, R., Mitchell, D. L., Argall, M. R., Bromund, K., Burch, J. L., Cohen, I. J., Galloy, M., Giles, B., Jaynes, A. N., Le Contel, O., Oka, M., Phan, T. D., Walsh, B. M., Westlake, J., Wilder, F. D., Bale, S. D., Livi, R., Pulupa, M., Whittlesey, P., DeWolfe, A., Harter, B., Lucas, E., Auster, U., Bonnell, J. W., Cully, C. M., Donovan, E., Ergun, R. E., Frey, H. U., Jackel, B., Keiling, A., Korth, H., McFadden, J. P., Nishimura, Y., Plaschke, F., Robert, P., Turner, D. L., Weygand, J. M., Candey, R. M., Johnson, R. C., Kovalick, T., Liu, M. H., McGuire, R. E., Breneman, A., Kersten, K., Schroeder, P., Angelopoulos, V., Cruce, P., Drozdov, A., Grimes, E. W., Hatzigeorgiu, N., King, D. A., Larson, D., Lewis, J. W., McTiernan, J. M., Roberts, D. A., Russell, C. L., Hori, T., Kasahara, Y., Kumamoto, A., Matsuoka, A., Miyashita, Y., Miyoshi, Y., Shinohara, I., Teramoto, M., Faden, J. B., Halford, A. J., McCarthy, M., Millan, R. M., Sample, J. G., Smith, D. M., Woodger, L. A., Masson, A., Narock, A. A., Asamura, K., Chang, T. F., Chiang, C.-Y., Kazama, Y., Keika, K., Matsuda, S., Segawa, T., Seki, K., Shoji, M., Tam, S. W. Y., Umemura, N., Wang, B.-J., Wang, S.-Y., Redmon, R., Rodriguez, J. V., Singer, H. J., Vandegriff, J., Abe, S., Nose, M., Shinbori, A., Tanaka, Y.-M., UeNo, S., Andersson, L., Dunn, P., Fowler, C., Halekas, J. S., Hara, T., Harada, Y., Lee, C. O., Lillis, R., Mitchell, D. L., Argall, M. R., Bromund, K., Burch, J. L., Cohen, I. J., Galloy, M., Giles, B., Jaynes, A. N., Le Contel, O., Oka, M., Phan, T. D., Walsh, B. M., Westlake, J., Wilder, F. D., Bale, S. D., Livi, R., Pulupa, M., Whittlesey, P., DeWolfe, A., Harter, B., Lucas, E., Auster, U., Bonnell, J. W., Cully, C. M., Donovan, E., Ergun, R. E., Frey, H. U., Jackel, B., Keiling, A., Korth, H., McFadden, J. P., Nishimura, Y., Plaschke, F., Robert, P., Turner, D. L., Weygand, J. M., Candey, R. M., Johnson, R. C., Kovalick, T., Liu, M. H., McGuire, R. E., Breneman, A., Kersten, K., and Schroeder, P.

Abstract

With the advent of the Heliophysics/Geospace System Observatory (H/GSO), a complement of multi-spacecraft missions and ground-based observatories to study the space environment, data retrieval, analysis, and visualization of space physics data can be daunting. The Space Physics Environment Data Analysis System (SPEDAS), a grass-roots software development platform (www.spedas.org), is now officially supported by NASA Heliophysics as part of its data environment infrastructure. It serves more than a dozen space missions and ground observatories and can integrate the full complement of past and upcoming space physics missions with minimal resources, following clear, simple, and well-proven guidelines. Free, modular and configurable to the needs of individual missions, it works in both command-line (ideal for experienced users) and Graphical User Interface (GUI) mode (reducing the learning curve for first-time users). Both options have “crib-sheets, ” user-command sequences in ASCII format that can facilitate record-and-repeat actions, especially for complex operations and plotting. Crib-sheets enhance scientific interactions, as users can move rapidly and accurately from exchanges of technical information on data processing to efficient discussions regarding data interpretation and science. SPEDAS can readily query and ingest all International Solar Terrestrial Physics (ISTP)-compatible products from the Space Physics Data Facility (SPDF), enabling access to a vast collection of historic and current mission data. The planned incorporation of Heliophysics Application Programmer’s Interface (HAPI) standards will facilitate data ingestion from distributed datasets that adhere to these standards. Although SPEDAS is currently Interactive Data Language (IDL)-based (and interfaces to Java-based tools such as Autoplot), efforts are under-way to expand it further to work with python (first as an interface tool and potentially even receiving an under-the-hood replacement). We re

Published
2019

2. The Space Physics Environment Data Analysis System (SPEDAS).

Author

Angelopoulos, V, Angelopoulos, V, Cruce, P, Drozdov, A, Grimes, EW, Hatzigeorgiu, N, King, DA, Larson, D, Lewis, JW, McTiernan, JM, Roberts, DA, Russell, CL, Hori, T, Kasahara, Y, Kumamoto, A, Matsuoka, A, Miyashita, Y, Miyoshi, Y, Shinohara, I, Teramoto, M, Faden, JB, Halford, AJ, McCarthy, M, Millan, RM, Sample, JG, Smith, DM, Woodger, LA, Masson, A, Narock, AA, Asamura, K, Chang, TF, Chiang, C-Y, Kazama, Y, Keika, K, Matsuda, S, Segawa, T, Seki, K, Shoji, M, Tam, SWY, Umemura, N, Wang, B-J, Wang, S-Y, Redmon, R, Rodriguez, JV, Singer, HJ, Vandegriff, J, Abe, S, Nose, M, Shinbori, A, Tanaka, Y-M, UeNo, S, Andersson, L, Dunn, P, Fowler, C, Halekas, JS, Hara, T, Harada, Y, Lee, CO, Lillis, R, Mitchell, DL, Argall, MR, Bromund, K, Burch, JL, Cohen, IJ, Galloy, M, Giles, B, Jaynes, AN, Le Contel, O, Oka, M, Phan, TD, Walsh, BM, Westlake, J, Wilder, FD, Bale, SD, Livi, R, Pulupa, M, Whittlesey, P, DeWolfe, A, Harter, B, Lucas, E, Auster, U, Bonnell, JW, Cully, CM, Donovan, E, Ergun, RE, Frey, HU, Jackel, B, Keiling, A, Korth, H, McFadden, JP, Nishimura, Y, Plaschke, F, Robert, P, Turner, DL, Weygand, JM, Candey, RM, Johnson, RC, Kovalick, T, Liu, MH, McGuire, RE, Breneman, A, Angelopoulos, V, Angelopoulos, V, Cruce, P, Drozdov, A, Grimes, EW, Hatzigeorgiu, N, King, DA, Larson, D, Lewis, JW, McTiernan, JM, Roberts, DA, Russell, CL, Hori, T, Kasahara, Y, Kumamoto, A, Matsuoka, A, Miyashita, Y, Miyoshi, Y, Shinohara, I, Teramoto, M, Faden, JB, Halford, AJ, McCarthy, M, Millan, RM, Sample, JG, Smith, DM, Woodger, LA, Masson, A, Narock, AA, Asamura, K, Chang, TF, Chiang, C-Y, Kazama, Y, Keika, K, Matsuda, S, Segawa, T, Seki, K, Shoji, M, Tam, SWY, Umemura, N, Wang, B-J, Wang, S-Y, Redmon, R, Rodriguez, JV, Singer, HJ, Vandegriff, J, Abe, S, Nose, M, Shinbori, A, Tanaka, Y-M, UeNo, S, Andersson, L, Dunn, P, Fowler, C, Halekas, JS, Hara, T, Harada, Y, Lee, CO, Lillis, R, Mitchell, DL, Argall, MR, Bromund, K, Burch, JL, Cohen, IJ, Galloy, M, Giles, B, Jaynes, AN, Le Contel, O, Oka, M, Phan, TD, Walsh, BM, Westlake, J, Wilder, FD, Bale, SD, Livi, R, Pulupa, M, Whittlesey, P, DeWolfe, A, Harter, B, Lucas, E, Auster, U, Bonnell, JW, Cully, CM, Donovan, E, Ergun, RE, Frey, HU, Jackel, B, Keiling, A, Korth, H, McFadden, JP, Nishimura, Y, Plaschke, F, Robert, P, Turner, DL, Weygand, JM, Candey, RM, Johnson, RC, Kovalick, T, Liu, MH, McGuire, RE, and Breneman, A

Abstract

With the advent of the Heliophysics/Geospace System Observatory (H/GSO), a complement of multi-spacecraft missions and ground-based observatories to study the space environment, data retrieval, analysis, and visualization of space physics data can be daunting. The Space Physics Environment Data Analysis System (SPEDAS), a grass-roots software development platform (www.spedas.org), is now officially supported by NASA Heliophysics as part of its data environment infrastructure. It serves more than a dozen space missions and ground observatories and can integrate the full complement of past and upcoming space physics missions with minimal resources, following clear, simple, and well-proven guidelines. Free, modular and configurable to the needs of individual missions, it works in both command-line (ideal for experienced users) and Graphical User Interface (GUI) mode (reducing the learning curve for first-time users). Both options have "crib-sheets," user-command sequences in ASCII format that can facilitate record-and-repeat actions, especially for complex operations and plotting. Crib-sheets enhance scientific interactions, as users can move rapidly and accurately from exchanges of technical information on data processing to efficient discussions regarding data interpretation and science. SPEDAS can readily query and ingest all International Solar Terrestrial Physics (ISTP)-compatible products from the Space Physics Data Facility (SPDF), enabling access to a vast collection of historic and current mission data. The planned incorporation of Heliophysics Application Programmer's Interface (HAPI) standards will facilitate data ingestion from distributed datasets that adhere to these standards. Although SPEDAS is currently Interactive Data Language (IDL)-based (and interfaces to Java-based tools such as Autoplot), efforts are under-way to expand it further to work with python (first as an interface tool and potentially even receiving an under-the-hood replacemen

Published
2019

3. The Space Physics Environment Data Analysis System (SPEDAS).

Author

Angelopoulos, V, Angelopoulos, V, Cruce, P, Drozdov, A, Grimes, EW, Hatzigeorgiu, N, King, DA, Larson, D, Lewis, JW, McTiernan, JM, Roberts, DA, Russell, CL, Hori, T, Kasahara, Y, Kumamoto, A, Matsuoka, A, Miyashita, Y, Miyoshi, Y, Shinohara, I, Teramoto, M, Faden, JB, Halford, AJ, McCarthy, M, Millan, RM, Sample, JG, Smith, DM, Woodger, LA, Masson, A, Narock, AA, Asamura, K, Chang, TF, Chiang, C-Y, Kazama, Y, Keika, K, Matsuda, S, Segawa, T, Seki, K, Shoji, M, Tam, SWY, Umemura, N, Wang, B-J, Wang, S-Y, Redmon, R, Rodriguez, JV, Singer, HJ, Vandegriff, J, Abe, S, Nose, M, Shinbori, A, Tanaka, Y-M, UeNo, S, Andersson, L, Dunn, P, Fowler, C, Halekas, JS, Hara, T, Harada, Y, Lee, CO, Lillis, R, Mitchell, DL, Argall, MR, Bromund, K, Burch, JL, Cohen, IJ, Galloy, M, Giles, B, Jaynes, AN, Le Contel, O, Oka, M, Phan, TD, Walsh, BM, Westlake, J, Wilder, FD, Bale, SD, Livi, R, Pulupa, M, Whittlesey, P, DeWolfe, A, Harter, B, Lucas, E, Auster, U, Bonnell, JW, Cully, CM, Donovan, E, Ergun, RE, Frey, HU, Jackel, B, Keiling, A, Korth, H, McFadden, JP, Nishimura, Y, Plaschke, F, Robert, P, Turner, DL, Weygand, JM, Candey, RM, Johnson, RC, Kovalick, T, Liu, MH, McGuire, RE, Breneman, A, Angelopoulos, V, Angelopoulos, V, Cruce, P, Drozdov, A, Grimes, EW, Hatzigeorgiu, N, King, DA, Larson, D, Lewis, JW, McTiernan, JM, Roberts, DA, Russell, CL, Hori, T, Kasahara, Y, Kumamoto, A, Matsuoka, A, Miyashita, Y, Miyoshi, Y, Shinohara, I, Teramoto, M, Faden, JB, Halford, AJ, McCarthy, M, Millan, RM, Sample, JG, Smith, DM, Woodger, LA, Masson, A, Narock, AA, Asamura, K, Chang, TF, Chiang, C-Y, Kazama, Y, Keika, K, Matsuda, S, Segawa, T, Seki, K, Shoji, M, Tam, SWY, Umemura, N, Wang, B-J, Wang, S-Y, Redmon, R, Rodriguez, JV, Singer, HJ, Vandegriff, J, Abe, S, Nose, M, Shinbori, A, Tanaka, Y-M, UeNo, S, Andersson, L, Dunn, P, Fowler, C, Halekas, JS, Hara, T, Harada, Y, Lee, CO, Lillis, R, Mitchell, DL, Argall, MR, Bromund, K, Burch, JL, Cohen, IJ, Galloy, M, Giles, B, Jaynes, AN, Le Contel, O, Oka, M, Phan, TD, Walsh, BM, Westlake, J, Wilder, FD, Bale, SD, Livi, R, Pulupa, M, Whittlesey, P, DeWolfe, A, Harter, B, Lucas, E, Auster, U, Bonnell, JW, Cully, CM, Donovan, E, Ergun, RE, Frey, HU, Jackel, B, Keiling, A, Korth, H, McFadden, JP, Nishimura, Y, Plaschke, F, Robert, P, Turner, DL, Weygand, JM, Candey, RM, Johnson, RC, Kovalick, T, Liu, MH, McGuire, RE, and Breneman, A

Abstract

With the advent of the Heliophysics/Geospace System Observatory (H/GSO), acomplement of multi-spacecraft missions and ground-based observatories to study the space environment, data retrieval, analysis, and visualization of space physics data can be daunting. The Space Physics Environment Data Analysis System (SPEDAS), agrass-roots software development platform (www.spedas.org), is now officially supported by NASA Heliophysics as part of its data environment infrastructure. It serves more than a dozen space missions and ground observatories and can integrate the full complement of past and upcoming space physics missions with minimal resources, following clear, simple, and well-proven guidelines. Free, modular and configurable to the needs of individual missions, it works in both command-line (ideal for experienced users) and Graphical User Interface (GUI) mode (reducing the learning curve for first-time users). Both options have "crib-sheets," user-command sequences in ASCII format that can facilitate record-and-repeat actions, especially for complex operations and plotting. Crib-sheets enhance scientific interactions, as users can move rapidly and accurately from exchanges of technical information on data processing to efficient discussions regarding data interpretation and science. SPEDAS can readily query and ingest all International Solar Terrestrial Physics (ISTP)-compatible products from the Space Physics Data Facility (SPDF), enabling access to a vast collection of historic and current mission data. The planned incorporation of Heliophysics Application Programmer's Interface (HAPI) standards will facilitate data ingestion from distributed datasets that adhere to these standards. Although SPEDAS is currently Interactive Data Language (IDL)-based (and interfaces to Java-based tools such as Autoplot), efforts are under-way to expand it further to work with python (first as an interface tool and potentially even receiving an under-the-hood replacement). We rev

Published
2019

4. The Space Physics Environment Data Analysis System (SPEDAS).

Author

Angelopoulos, V, Angelopoulos, V, Cruce, P, Drozdov, A, Grimes, EW, Hatzigeorgiu, N, King, DA, Larson, D, Lewis, JW, McTiernan, JM, Roberts, DA, Russell, CL, Hori, T, Kasahara, Y, Kumamoto, A, Matsuoka, A, Miyashita, Y, Miyoshi, Y, Shinohara, I, Teramoto, M, Faden, JB, Halford, AJ, McCarthy, M, Millan, RM, Sample, JG, Smith, DM, Woodger, LA, Masson, A, Narock, AA, Asamura, K, Chang, TF, Chiang, C-Y, Kazama, Y, Keika, K, Matsuda, S, Segawa, T, Seki, K, Shoji, M, Tam, SWY, Umemura, N, Wang, B-J, Wang, S-Y, Redmon, R, Rodriguez, JV, Singer, HJ, Vandegriff, J, Abe, S, Nose, M, Shinbori, A, Tanaka, Y-M, UeNo, S, Andersson, L, Dunn, P, Fowler, C, Halekas, JS, Hara, T, Harada, Y, Lee, CO, Lillis, R, Mitchell, DL, Argall, MR, Bromund, K, Burch, JL, Cohen, IJ, Galloy, M, Giles, B, Jaynes, AN, Le Contel, O, Oka, M, Phan, TD, Walsh, BM, Westlake, J, Wilder, FD, Bale, SD, Livi, R, Pulupa, M, Whittlesey, P, DeWolfe, A, Harter, B, Lucas, E, Auster, U, Bonnell, JW, Cully, CM, Donovan, E, Ergun, RE, Frey, HU, Jackel, B, Keiling, A, Korth, H, McFadden, JP, Nishimura, Y, Plaschke, F, Robert, P, Turner, DL, Weygand, JM, Candey, RM, Johnson, RC, Kovalick, T, Liu, MH, McGuire, RE, Breneman, A, Angelopoulos, V, Angelopoulos, V, Cruce, P, Drozdov, A, Grimes, EW, Hatzigeorgiu, N, King, DA, Larson, D, Lewis, JW, McTiernan, JM, Roberts, DA, Russell, CL, Hori, T, Kasahara, Y, Kumamoto, A, Matsuoka, A, Miyashita, Y, Miyoshi, Y, Shinohara, I, Teramoto, M, Faden, JB, Halford, AJ, McCarthy, M, Millan, RM, Sample, JG, Smith, DM, Woodger, LA, Masson, A, Narock, AA, Asamura, K, Chang, TF, Chiang, C-Y, Kazama, Y, Keika, K, Matsuda, S, Segawa, T, Seki, K, Shoji, M, Tam, SWY, Umemura, N, Wang, B-J, Wang, S-Y, Redmon, R, Rodriguez, JV, Singer, HJ, Vandegriff, J, Abe, S, Nose, M, Shinbori, A, Tanaka, Y-M, UeNo, S, Andersson, L, Dunn, P, Fowler, C, Halekas, JS, Hara, T, Harada, Y, Lee, CO, Lillis, R, Mitchell, DL, Argall, MR, Bromund, K, Burch, JL, Cohen, IJ, Galloy, M, Giles, B, Jaynes, AN, Le Contel, O, Oka, M, Phan, TD, Walsh, BM, Westlake, J, Wilder, FD, Bale, SD, Livi, R, Pulupa, M, Whittlesey, P, DeWolfe, A, Harter, B, Lucas, E, Auster, U, Bonnell, JW, Cully, CM, Donovan, E, Ergun, RE, Frey, HU, Jackel, B, Keiling, A, Korth, H, McFadden, JP, Nishimura, Y, Plaschke, F, Robert, P, Turner, DL, Weygand, JM, Candey, RM, Johnson, RC, Kovalick, T, Liu, MH, McGuire, RE, and Breneman, A

Abstract

With the advent of the Heliophysics/Geospace System Observatory (H/GSO), a complement of multi-spacecraft missions and ground-based observatories to study the space environment, data retrieval, analysis, and visualization of space physics data can be daunting. The Space Physics Environment Data Analysis System (SPEDAS), a grass-roots software development platform (www.spedas.org), is now officially supported by NASA Heliophysics as part of its data environment infrastructure. It serves more than a dozen space missions and ground observatories and can integrate the full complement of past and upcoming space physics missions with minimal resources, following clear, simple, and well-proven guidelines. Free, modular and configurable to the needs of individual missions, it works in both command-line (ideal for experienced users) and Graphical User Interface (GUI) mode (reducing the learning curve for first-time users). Both options have "crib-sheets," user-command sequences in ASCII format that can facilitate record-and-repeat actions, especially for complex operations and plotting. Crib-sheets enhance scientific interactions, as users can move rapidly and accurately from exchanges of technical information on data processing to efficient discussions regarding data interpretation and science. SPEDAS can readily query and ingest all International Solar Terrestrial Physics (ISTP)-compatible products from the Space Physics Data Facility (SPDF), enabling access to a vast collection of historic and current mission data. The planned incorporation of Heliophysics Application Programmer's Interface (HAPI) standards will facilitate data ingestion from distributed datasets that adhere to these standards. Although SPEDAS is currently Interactive Data Language (IDL)-based (and interfaces to Java-based tools such as Autoplot), efforts are under-way to expand it further to work with python (first as an interface tool and potentially even receiving an under-the-hood replacemen

Published
2019

5. Correction to: Simultaneous observation of auroral substorm onset in Polar satellite global images and ground-based all-sky images (Earth, Planets and Space, (2018), 70, 1, (73), 10.1186/s40623-018-0843-3)

Author

Ieda, A., Kauristie, K., Nishimura, Y., Miyashita, Y., Frey, H.U., Juusola, L., Whiter, D., Nosé, M., Fillingim, M.O., Honary, F., Rogers, N.C., Miyoshi, Y., Miura, T., Kawashima, T., Machida, S., Ieda, A., Kauristie, K., Nishimura, Y., Miyashita, Y., Frey, H.U., Juusola, L., Whiter, D., Nosé, M., Fillingim, M.O., Honary, F., Rogers, N.C., Miyoshi, Y., Miura, T., Kawashima, T., and Machida, S.

Abstract

In the original publication of this article [1], some reference lines are missing in Fig. 5a and Fig. 6b(6). This correction shows the correct figures. The publisher apologizes to the readers and authors for the inconvenience. The original publication has been corrected. © 2019, The Author(s).

Published
2019

6. Charge-changing cross sections of ^<30>Ne, ^<32,33>Na with a proton target

Author

Ozawa, A., Moriguchi, T., Ohtsubo, T., Aoi, N., Fang, D. Q., Fukuda, N., Fukuda, M., Geissel, H., Hachiuma, I., Inabe, N., Ishibashi, Y., Ishimoto, S., Ito, Y., Izumikawa, T., Kameda, D., Kubo, T., Kuboki, T., Kusaka, K., Lantz, M., Ma, Y. G., Mihara, M., Miyashita, Y., Momota, S., Nagae, D., Namihira, K., Nishimura, D., Ooishi, H., Ohkuma, Y., Ohnishi, T., Ohtake, M., Ogawa, K., Shimbara, Y., Suda, T., Sumikama, T., Suzuki, H., Suzuki, S., Suzuki, T., Takechi, M., Takeda, H., Tanaka, K., Watanabe, R., Winkler, M., Yamaguchi, T., Yanagisawa, Y., Yasuda, Y., Yoshinaga, K., Yoshida, A., Yoshida, K., Ozawa, A., Moriguchi, T., Ohtsubo, T., Aoi, N., Fang, D. Q., Fukuda, N., Fukuda, M., Geissel, H., Hachiuma, I., Inabe, N., Ishibashi, Y., Ishimoto, S., Ito, Y., Izumikawa, T., Kameda, D., Kubo, T., Kuboki, T., Kusaka, K., Lantz, M., Ma, Y. G., Mihara, M., Miyashita, Y., Momota, S., Nagae, D., Namihira, K., Nishimura, D., Ooishi, H., Ohkuma, Y., Ohnishi, T., Ohtake, M., Ogawa, K., Shimbara, Y., Suda, T., Sumikama, T., Suzuki, H., Suzuki, S., Suzuki, T., Takechi, M., Takeda, H., Tanaka, K., Watanabe, R., Winkler, M., Yamaguchi, T., Yanagisawa, Y., Yasuda, Y., Yoshinaga, K., Yoshida, A., and Yoshida, K.

Abstract

The total charge-changing, charge pick-up, and partial charge-changing cross sections of very neutron-rich nuclei (^<30>Ne, ^<32,33>Na) with a proton target have been measured at ∼240A MeV for the first time. We introduced the phenomenological correction factor in Glauber-model calculations for the total charge-changing cross sections with the proton target, and applied it to deduce the proton radii of these nuclei. For ^<30>Ne and ^<32>Na, the neutron skin thicknesses of the nuclei were deduced by comparing the proton radii with the matter radii deduced from the interaction cross-section measurements. A significant thick neutron-skin has been observed for the nuclei. We also found that the charge pick-up cross sections are much larger than those in the systematics of stable nuclei.

Published
2019

7. Correction to: Simultaneous observation of auroral substorm onset in Polar satellite global images and ground-based all-sky images (Earth, Planets and Space, (2018), 70, 1, (73), 10.1186/s40623-018-0843-3)

Author

Ieda, A., Kauristie, K., Nishimura, Y., Miyashita, Y., Frey, H.U., Juusola, L., Whiter, D., Nosé, M., Fillingim, M.O., Honary, F., Rogers, N.C., Miyoshi, Y., Miura, T., Kawashima, T., Machida, S., Ieda, A., Kauristie, K., Nishimura, Y., Miyashita, Y., Frey, H.U., Juusola, L., Whiter, D., Nosé, M., Fillingim, M.O., Honary, F., Rogers, N.C., Miyoshi, Y., Miura, T., Kawashima, T., and Machida, S.

Abstract

In the original publication of this article [1], some reference lines are missing in Fig. 5a and Fig. 6b(6). This correction shows the correct figures. The publisher apologizes to the readers and authors for the inconvenience. The original publication has been corrected. © 2019, The Author(s).

Published
2019

8. Electrostatic electron cyclotron harmonic waves as a candidate to cause pulsating auroras

Author

Fukizawa, M. (M.), Sakanoi, T. (T.), Miyoshi, Y. (Y.), Hosokawa, K. (K.), Shiokawa, K. (K.), Katoh, Y. (Y.), Kazama, Y. (Y.), Kumamoto, A. (A.), Tsuchiya, F. (F.), Miyashita, Y. (Y.), Tanaka, Y. -. (Y. -M.), Kasahara, Y. (Y.), Ozaki, M. (M.), Matsuoka, A. (A.), Matsuda, S. (S.), Hikishima, M. (M.), Oyama, S. (S.), Ogawa, Y. (Y.), Kurita, S. (S.), Fujii, R. (R.), Fukizawa, M. (M.), Sakanoi, T. (T.), Miyoshi, Y. (Y.), Hosokawa, K. (K.), Shiokawa, K. (K.), Katoh, Y. (Y.), Kazama, Y. (Y.), Kumamoto, A. (A.), Tsuchiya, F. (F.), Miyashita, Y. (Y.), Tanaka, Y. -. (Y. -M.), Kasahara, Y. (Y.), Ozaki, M. (M.), Matsuoka, A. (A.), Matsuda, S. (S.), Hikishima, M. (M.), Oyama, S. (S.), Ogawa, Y. (Y.), Kurita, S. (S.), and Fujii, R. (R.)

Abstract

Pulsating auroras (PsAs) are thought to be generated by precipitating electrons scattered by lower‐band chorus (LBC) waves near the magnetic equator. One‐to‐one correlation between the LBC intensity and the PsA intensity has been reported. Electrostatic electron cyclotron harmonic (ECH) waves can also scatter electrons. However, direct correlation between ECH and PsA has not been reported yet. In this study, using a coordinated Exploration of energization and Radiation in Geospace (Arase) satellite and ground‐based imager observation, we report that not only LBC but also ECH have correlation with PsA. We estimated the precipitating electron energy by assuming that the time lag when the cross‐correlation coefficient became the highest was travel time of electrons from the modulation region. We found that the estimated energies show reasonable values as the cyclotron resonance energy of each wave.

Published
2018

9. Large‐scale ducting of Pc1 pulsations observed by Swarm satellites and multiple ground networks

Author

Kim, H. (Hyangpyo), Hwang, J. (Junga), Park, J. (Jaeheung), Miyashita, Y. (Yukinaga), Shiokawa, K. (Kazuo), Mann, I. R. (Ian R.), Raita, T. (Tero), Lee, J. (Jaejin), Kim, H. (Hyangpyo), Hwang, J. (Junga), Park, J. (Jaeheung), Miyashita, Y. (Yukinaga), Shiokawa, K. (Kazuo), Mann, I. R. (Ian R.), Raita, T. (Tero), and Lee, J. (Jaejin)

Abstract

Low Earth orbit satellites frequently encounter Pc1 pulsations, but most have been observed with limited latitudinal extent or short lifetime. In this study we analyze two large‐scale Pc1 pulsations (both latitudinally wide and long‐lasting) generated by ionospheric ducting effect using Swarm and ground magnetometers on 25 June and 3 September 2015. Swarm observed the 25 June pulsations on both dayside and nightside during the storm time substorm (a strong geomagnetic storm on 23 June with \(D_{st} = − 204~nT\)). We found the Pc1 pulsations were pervasive in both magnetic local time sectors of dayside and nightside for at least 2 hr. Another large Pc1 pulsation on 3 September was observed during a nonstorm substorm period. We conclude that (1) ionospheric ducting can transmit Pc1 waves to a wide range of L shells, (2) geomagnetic storm is not a prerequisite for such large‐scale ducting, and (3) wave intensity can abruptly decrease across sharp gradients in the ionospheric plasma density.

Published
2018

10. Detection of Gamma Rays around 1 TeV from RX J0852.0-4622 by CANGAROO-II

Author

片桐, 秀明, 榎本, 良治, Ksenofontov, L. T., 森, 正樹, 足立, 裕樹, 浅原, 明広, Bicknell, G. V., Clay, R. W., 土井, 康博, Edwards, P. G., 郡司, 修一, 原, 敏, 原, 忠生, 服部, 敬裕, 林, 清一, 伊藤, 千枝, 株木, 重人, 梶野, 文義, 河内, 明子, 木船, 正, 木内, 隆太, 窪, 秀利, Kurihara, T., Kurosaka, R., 櫛田, 淳子, 松原, 豊, Miyashita, Y., 水本, 好彦, 村石, 浩, 村木, やすし, Katagiri, H., Enomoto, R., Mori, M., Adachi, Y., Asahara, A., Doi, Y., Gunji, S., Hara, S., Hara, T., Hattori, T., Hayashi, Seiichi, Itoh, Chie, Kabuki, S., Kajino, F., Kawachi, Akiko, Kifune, T., Kiuchi, R., Kubo, Hidetoshi, Kushida, J., Matsubara, Y., Mizumoto, Y., Muraishi, H., Muraki, Y., 片桐, 秀明, 榎本, 良治, Ksenofontov, L. T., 森, 正樹, 足立, 裕樹, 浅原, 明広, Bicknell, G. V., Clay, R. W., 土井, 康博, Edwards, P. G., 郡司, 修一, 原, 敏, 原, 忠生, 服部, 敬裕, 林, 清一, 伊藤, 千枝, 株木, 重人, 梶野, 文義, 河内, 明子, 木船, 正, 木内, 隆太, 窪, 秀利, Kurihara, T., Kurosaka, R., 櫛田, 淳子, 松原, 豊, Miyashita, Y., 水本, 好彦, 村石, 浩, 村木, やすし, Katagiri, H., Enomoto, R., Mori, M., Adachi, Y., Asahara, A., Doi, Y., Gunji, S., Hara, S., Hara, T., Hattori, T., Hayashi, Seiichi, Itoh, Chie, Kabuki, S., Kajino, F., Kawachi, Akiko, Kifune, T., Kiuchi, R., Kubo, Hidetoshi, Kushida, J., Matsubara, Y., Mizumoto, Y., Muraishi, H., and Muraki, Y.

Abstract

著者人数: 51名, Accepted: 2004-12-10

Published
2015

11. Magnetic reconnection X-line retreat associated with dipolarization of the Earth's magnetosphere

Author

Oka, M., Phan, T.-D., Eastwood, J. P., Angelopoulos, V., Murphy, N. A., Oieroset, M., 宮下, 幸長, 藤本, 正樹, McFadden, J., Larson, D., Miyashita, Y., Fujimoto, Masaki, Oka, M., Phan, T.-D., Eastwood, J. P., Angelopoulos, V., Murphy, N. A., Oieroset, M., 宮下, 幸長, 藤本, 正樹, McFadden, J., Larson, D., Miyashita, Y., and Fujimoto, Masaki

Abstract

Accepted: 2011-09-13

Published
2015

12. Plasmoids Observed in the near-Earth Magnetotail at X - -7 RE

Author

宮下, 幸長, 家田, 章正, 上出, 洋介, 町田, 忍, 向井, 利典, 齋藤, 義文, Liou, K., Meng, C.-I., Parks, G. K., McEntire, R. W., 西谷, 望, Lester, M., Sofko, G. J., Villain, J.-P., Miyashita, Y., Ieda, A., Kamide, Y., Machida, S., Mukai, Toshifumi, Saito, Yoshifumi, Nishitani, N., 宮下, 幸長, 家田, 章正, 上出, 洋介, 町田, 忍, 向井, 利典, 齋藤, 義文, Liou, K., Meng, C.-I., Parks, G. K., McEntire, R. W., 西谷, 望, Lester, M., Sofko, G. J., Villain, J.-P., Miyashita, Y., Ieda, A., Kamide, Y., Machida, S., Mukai, Toshifumi, Saito, Yoshifumi, and Nishitani, N.

Abstract

著者人数：14名, Accepted: 2005-09-22

Published
2015

13. Difference in magnetotail variations between intense and weak substorms

Author

宮下, 幸長, 上出, 洋介, 町田, 忍, Liou, K., 向井, 利典, 齋藤, 義文, 家田, 章正, Meng, C.-I., Parks, G. K., Miyashita, Y., Kamide, Y., Machida, S., Mukai, Toshifumi, Saito, Yoshifumi, Ieda, A., 宮下, 幸長, 上出, 洋介, 町田, 忍, Liou, K., 向井, 利典, 齋藤, 義文, 家田, 章正, Meng, C.-I., Parks, G. K., Miyashita, Y., Kamide, Y., Machida, S., Mukai, Toshifumi, Saito, Yoshifumi, and Ieda, A.

Abstract

Accepted: 2004-08-24

Published
2015

14. Charge-changing cross sections of 30Ne, 32,33Na with a proton target

Author

Ozawa, A., Moriguchi, T., Ohtsubo, T., Aoi, N., Fang, D. Q., Fukuda, N., Fukuda, M., Geissel, H., Hachiuma, I., Inabe, N., Ishibashi, Y., Ishimoto, S., Ito, Y., Izumikawa, T., Kameda, D., Kubo, T., Kuboki, T., Kusaka, K., Lantz, Mattias, Ma, Y. G., Mihara, M., Miyashita, Y., Momota, S., Nagae, D., Namihira, K., Nishimura, D., Ooishi, H., Ohkuma, Y., Ohnishi, T., Ohtake, M., Ogawa, K., Shimbara, Y., Suda, T., Sumikama, T., Suzuki, H., Suzuki, S., Suzuki, T., Takechi, M., Takeda, H., Tanaka, K., Watanabe, R., Winkler, M., Yamaguchi, T., Yanagisawa, Y., Yasuda, Y., Yoshinaga, K., Yoshida, A., Yoshida, K., Ozawa, A., Moriguchi, T., Ohtsubo, T., Aoi, N., Fang, D. Q., Fukuda, N., Fukuda, M., Geissel, H., Hachiuma, I., Inabe, N., Ishibashi, Y., Ishimoto, S., Ito, Y., Izumikawa, T., Kameda, D., Kubo, T., Kuboki, T., Kusaka, K., Lantz, Mattias, Ma, Y. G., Mihara, M., Miyashita, Y., Momota, S., Nagae, D., Namihira, K., Nishimura, D., Ooishi, H., Ohkuma, Y., Ohnishi, T., Ohtake, M., Ogawa, K., Shimbara, Y., Suda, T., Sumikama, T., Suzuki, H., Suzuki, S., Suzuki, T., Takechi, M., Takeda, H., Tanaka, K., Watanabe, R., Winkler, M., Yamaguchi, T., Yanagisawa, Y., Yasuda, Y., Yoshinaga, K., Yoshida, A., and Yoshida, K.

Abstract

The total charge-changing, charge pick-up, and partial charge-changing cross sections of very neutron-rich nuclei (30Ne, 32,33Na) with a proton target have been measured at ~240A MeV for the first time. We introduced the phenomenological correction factor in Glauber-model calculations for the total charge-changing cross sections with the proton target, and applied it to deduce the proton radii of these nuclei. For 30Ne and 32Na, the neutron skin thicknesses of the nuclei were deduced by comparing the proton radii with the matter radii deduced from the interaction cross-section measurements. A significant thick neutron-skin has been observed for the nuclei. We also found that the charge pick-up cross sections are much larger than those in the systematics of stable nuclei.

Published
2014
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15. Charge-changing cross sections of ^<30>Ne, ^<32,33>Na with a proton target

Author

Ozawa, A., Moriguchi, T., Ohtsubo, T., Aoi, N., Fang, D. Q., Fukuda, N., Fukuda, M., Geissel, H., Hachiuma, I., Inabe, N., Ishibashi, Y., Ishimoto, S., Ito, Y., Izumikawa, T., Kameda, D., Kubo, T., Kuboki, T., Kusaka, K., Lantz, M., Ma, Y. G., Mihara, M., Miyashita, Y., Momota, S., Nagae, D., Namihira, K., Nishimura, D., Ooishi, H., Ohkuma, Y., Ohnishi, T., Ohtake, M., Ogawa, K., Shimbara, Y., Suda, T., Sumikama, T., Suzuki, H., Suzuki, S., Suzuki, T., Takechi, M., Takeda, H., Tanaka, K., Watanabe, R., Winkler, M., Yamaguchi, T., Yanagisawa, Y., Yasuda, Y., Yoshinaga, K., Yoshida, A., Yoshida, K., Ozawa, A., Moriguchi, T., Ohtsubo, T., Aoi, N., Fang, D. Q., Fukuda, N., Fukuda, M., Geissel, H., Hachiuma, I., Inabe, N., Ishibashi, Y., Ishimoto, S., Ito, Y., Izumikawa, T., Kameda, D., Kubo, T., Kuboki, T., Kusaka, K., Lantz, M., Ma, Y. G., Mihara, M., Miyashita, Y., Momota, S., Nagae, D., Namihira, K., Nishimura, D., Ooishi, H., Ohkuma, Y., Ohnishi, T., Ohtake, M., Ogawa, K., Shimbara, Y., Suda, T., Sumikama, T., Suzuki, H., Suzuki, S., Suzuki, T., Takechi, M., Takeda, H., Tanaka, K., Watanabe, R., Winkler, M., Yamaguchi, T., Yanagisawa, Y., Yasuda, Y., Yoshinaga, K., Yoshida, A., and Yoshida, K.

Abstract

The total charge-changing, charge pick-up, and partial charge-changing cross sections of very neutron-rich nuclei (^<30>Ne, ^<32,33>Na) with a proton target have been measured at ∼240A MeV for the first time. We introduced the phenomenological correction factor in Glauber-model calculations for the total charge-changing cross sections with the proton target, and applied it to deduce the proton radii of these nuclei. For ^<30>Ne and ^<32>Na, the neutron skin thicknesses of the nuclei were deduced by comparing the proton radii with the matter radii deduced from the interaction cross-section measurements. A significant thick neutron-skin has been observed for the nuclei. We also found that the charge pick-up cross sections are much larger than those in the systematics of stable nuclei., journal article

Published
2014

16. Interaction cross sections for Ne isotopes towards the island of inversion and halo structures of 29Ne and 31Ne

Author

Takechi, M., Ohtsubo, T., Fukuda, M., Nishimura, D., Kuboki, T., Suzuki, T., Yamaguchi, T., Ozawa, A., Moriguchi, T., Ooishi, H., Nagae, D., Suzuki, H., Suzuki, S., Izumikawa, T., Sumikama, T., Ishihara, M., Geissel, H., Aoi, N., Chen, Rui-Jiu, Fang, De-Qing, Fukuda, N., Hachiuma, I., Inabe, N., Ishibashi, Y., Ito, Y., Kameda, D., Kubo, T., Kusaka, K., Lantz, Mattias, Ma, Yu-Gang, Matsuta, K., Mihara, M., Miyashita, Y., Momota, S., Namihira, K., Nagashima, M., Ohkuma, Y., Ohnishi, T., Ohtake, M., Ogawa, K., Sakurai, H., Shimbara, Y., Suda, T., Takeda, H., Takeuchi, S., Tanaka, K., Watanabe, R., Winkler, M., Yanagisawa, Y., Yasuda, Y., Yoshinaga, K., Yoshida, A., Yoshida, K., Takechi, M., Ohtsubo, T., Fukuda, M., Nishimura, D., Kuboki, T., Suzuki, T., Yamaguchi, T., Ozawa, A., Moriguchi, T., Ooishi, H., Nagae, D., Suzuki, H., Suzuki, S., Izumikawa, T., Sumikama, T., Ishihara, M., Geissel, H., Aoi, N., Chen, Rui-Jiu, Fang, De-Qing, Fukuda, N., Hachiuma, I., Inabe, N., Ishibashi, Y., Ito, Y., Kameda, D., Kubo, T., Kusaka, K., Lantz, Mattias, Ma, Yu-Gang, Matsuta, K., Mihara, M., Miyashita, Y., Momota, S., Namihira, K., Nagashima, M., Ohkuma, Y., Ohnishi, T., Ohtake, M., Ogawa, K., Sakurai, H., Shimbara, Y., Suda, T., Takeda, H., Takeuchi, S., Tanaka, K., Watanabe, R., Winkler, M., Yanagisawa, Y., Yasuda, Y., Yoshinaga, K., Yoshida, A., and Yoshida, K.

Abstract

Interaction cross sections (σI) for Ne isotopes from the stability line to the vicinity of the neutron dripline have been measured at around 240 MeV/nucleon using BigRIPS at RIBF, RIKEN. The σI for 27–32Ne in every case exceed the systematic mass-number dependence of σI for stable nuclei, which can be explained by considering the nuclear deformation. In particular the σI for 29Ne and 31Ne are significantly greater than those of their neighboring nuclides. These enhancements of σI for 29Ne and 31Ne cannot be explained by a single-particle model calculation under the assumption that the valence neutron of 29Ne (31Ne) occupies the 0d3/2 (0f7/2 ) orbital, as expected from the standard spherical shell ordering. The present data suggest an s dominant halo structure of 29Ne and s- or p-orbital halo in 31Ne.

Published
2012
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17. The energization and radiation in geospace (ERG) project

Author

Miyoshi, Y., Ono, T., Takashima, T., Asamura, K., Hirahara, M., Kasaba, Y., Matsuoka, A., Kojima, H., Shiokawa, K., Seki, K., Fujimoto, M., Nagatsuma, T., Cheng, C. Z., Kazama, Y., Kasahara, S., Mitani, T., Matsumoto, H., Higashio, N., Kumamoto, A., Yagitani, S., Kasahara, Y., Ishisaka, K., Blomberg, Lars, Fujimoto, A., Katoh, Y., Ebihara, Y., Omura, Y., Nosé, M., Hori, T., Miyashita, Y., Tanaka, Y. -M, Segawa, T., Miyoshi, Y., Ono, T., Takashima, T., Asamura, K., Hirahara, M., Kasaba, Y., Matsuoka, A., Kojima, H., Shiokawa, K., Seki, K., Fujimoto, M., Nagatsuma, T., Cheng, C. Z., Kazama, Y., Kasahara, S., Mitani, T., Matsumoto, H., Higashio, N., Kumamoto, A., Yagitani, S., Kasahara, Y., Ishisaka, K., Blomberg, Lars, Fujimoto, A., Katoh, Y., Ebihara, Y., Omura, Y., Nosé, M., Hori, T., Miyashita, Y., Tanaka, Y. -M, and Segawa, T.

Abstract

The Energization and Radiation in Geospace (ERG) project for solar cycle 24 will explore how relativistic electrons in the radiation belts are generated during space storms. This geospace exploration project consists of three research teams: the ERG satellite observation team, the ground-based network observation team, and the integrated data analysis/simulation team. Satellite observation will provide in situ measurements of features such as the plasma distribution function, electric and magnetic fields, and plasma waves, whereas remote sensing by ground-based observations using, for example, HF radars, magnetometers, optical instruments, and radio wave receivers will provide the global state of the geospace. Various kinds of data will be integrated and compared with numerical simulations for quantitative understanding. Such a synergetic approach is essential for comprehensive understanding of relativistic electron generation/loss processes through crossenergy and cross-regional coupling in which different plasma populations and regions are dynamically coupled with each other. In addition, the ERG satellite will utilize a new and innovative measurement technique for wave-particle interactions that can directly measure the energy exchange process between particles and plasma waves. In this paper, we briefly review some of the profound problems regarding relativistic electron accelerations and losses that will be solved by the ERG project, and we provide an overview of the project., QC 20150306

Published
2012
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18. Structural Evolution in the Neutron-Rich Nuclei Zr-106 and Zr-108

Author

Sumikama, T, Yoshinaga, K, Watanabe, H, Nishimura, S, Miyashita, Y, Yamaguchi, K, Sugimoto, K, Chiba, J, Li, Z, Baba, H, Berryman, JS, Blasi, N, Bracco, A, Camera, F, Doornenbal, P, Go, S, Hashimoto, T, Hayakawa, S, Hinke, C, Ideguchi, E, Isobe, T, Ito, Y, Jenkins, DG, Kawada, Y, Kobayashi, N, Kondo, Y, Kruecken, R, Kubono, S, Lorusso, G, Nakano, T, Kurata-Nishimura, M, Odahara, A, Ong, HJ, Ota, S, Podolyak, Z, Sakurai, H, Scheit, H, Steiger, K, Steppenbeck, D, Takano, S, Takashima, A, Tajiri, K, Teranishi, T, Wakabayashi, Y, Walker, PM, Wieland, O, Yamaguchi, H, Sumikama, T, Yoshinaga, K, Watanabe, H, Nishimura, S, Miyashita, Y, Yamaguchi, K, Sugimoto, K, Chiba, J, Li, Z, Baba, H, Berryman, JS, Blasi, N, Bracco, A, Camera, F, Doornenbal, P, Go, S, Hashimoto, T, Hayakawa, S, Hinke, C, Ideguchi, E, Isobe, T, Ito, Y, Jenkins, DG, Kawada, Y, Kobayashi, N, Kondo, Y, Kruecken, R, Kubono, S, Lorusso, G, Nakano, T, Kurata-Nishimura, M, Odahara, A, Ong, HJ, Ota, S, Podolyak, Z, Sakurai, H, Scheit, H, Steiger, K, Steppenbeck, D, Takano, S, Takashima, A, Tajiri, K, Teranishi, T, Wakabayashi, Y, Walker, PM, Wieland, O, and Yamaguchi, H

Published
2011

19. Development of axial asymmetry in the neutron-rich nucleus Mo-110

Author

Watanabe, H, Yamaguchi, K, Odahara, A, Sumikama, T, Nishimura, S, Yoshinaga, K, Li, Z, Miyashita, Y, Sato, K, Prochniak, L, Baba, H, Berryman, JS, Blasi, N, Bracco, A, Camera, F, Chiba, J, Doornenbal, P, Go, S, Hashimoto, T, Hayakawa, S, Hinke, C, Hinohara, N, Ideguchi, E, Isobe, T, Ito, Y, Jenkins, DG, Kawada, Y, Kobayashi, N, Kondo, Y, Kruecken, R, Kubono, S, Lorusso, G, Nakano, T, Nakatsukasa, T, Kurata-Nishimura, M, Ong, HJ, Ota, S, Podolyak, Z, Sakurai, H, Scheit, H, Steiger, K, Steppenbeck, D, Sugimoto, K, Tajiri, K, Takano, S, Takashima, A, Teranishi, T, Wakabayashi, Y, Walker, PM, Wieland, O, Yamaguchi, H, Watanabe, H, Yamaguchi, K, Odahara, A, Sumikama, T, Nishimura, S, Yoshinaga, K, Li, Z, Miyashita, Y, Sato, K, Prochniak, L, Baba, H, Berryman, JS, Blasi, N, Bracco, A, Camera, F, Chiba, J, Doornenbal, P, Go, S, Hashimoto, T, Hayakawa, S, Hinke, C, Hinohara, N, Ideguchi, E, Isobe, T, Ito, Y, Jenkins, DG, Kawada, Y, Kobayashi, N, Kondo, Y, Kruecken, R, Kubono, S, Lorusso, G, Nakano, T, Nakatsukasa, T, Kurata-Nishimura, M, Ong, HJ, Ota, S, Podolyak, Z, Sakurai, H, Scheit, H, Steiger, K, Steppenbeck, D, Sugimoto, K, Tajiri, K, Takano, S, Takashima, A, Teranishi, T, Wakabayashi, Y, Walker, PM, Wieland, O, and Yamaguchi, H

Published
2011

20. Low-lying level structure of the neutron-rich nucleus 109Nb: A possible oblate-shape isomer

Author

Watanabe, H, Sumikama, T, Nishimura, S, Yoshinaga, K, Li, Z, Miyashita, Y, Yamaguchi, K, Baba, H, Berryman, JS, Blasi, N, Bracco, A, Camera, F, Chiba, J, Doornenbal, P, Go, S, Hashimoto, T, Hayakawa, S, Hinke, C, Ideguchi, E, Isobe, T, Ito, Y, Jenkins, DG, Kawada, Y, Kobayashi, N, Kondo, Y, Krücken, R, Kubono, S, Lorusso, G, Nakano, T, Kurata-Nishimura, M, Odahara, A, Ong, HJ, Ota, S, Podolyák, Z, Sakurai, H, Scheit, H, Shi, Y, Steiger, K, Steppenbeck, D, Sugimoto, K, Tajiri, K, Takano, S, Takashima, A, Teranishi, T, Wakabayashi, Y, Walker, PM, Wieland, O, Xu, FR, Yamaguchi, H, Watanabe, H, Sumikama, T, Nishimura, S, Yoshinaga, K, Li, Z, Miyashita, Y, Yamaguchi, K, Baba, H, Berryman, JS, Blasi, N, Bracco, A, Camera, F, Chiba, J, Doornenbal, P, Go, S, Hashimoto, T, Hayakawa, S, Hinke, C, Ideguchi, E, Isobe, T, Ito, Y, Jenkins, DG, Kawada, Y, Kobayashi, N, Kondo, Y, Krücken, R, Kubono, S, Lorusso, G, Nakano, T, Kurata-Nishimura, M, Odahara, A, Ong, HJ, Ota, S, Podolyák, Z, Sakurai, H, Scheit, H, Shi, Y, Steiger, K, Steppenbeck, D, Sugimoto, K, Tajiri, K, Takano, S, Takashima, A, Teranishi, T, Wakabayashi, Y, Walker, PM, Wieland, O, Xu, FR, and Yamaguchi, H

Published
2011

21. Measurements of nuclear radii for neutron-rich Ne isotopes 28-32Ne

Author

Takechi, M., Ohtsubo, T., Kuboki, T., Fukuda, M., Nishimura, D., Suzuki, T., Yamaguchi, T., Ozawa, A., Moriguchi, T., Sumikama, T., Geissel, H., Aoi, N., Fukuda, N., Hachiuma, I., Inabe, N., Ishibashi, Y., Itoh, Y., Kameda, D., Kusaka, K., Lantz, Mattias, Mihara, M., Miyashita, Y., Momota, S., Namihira, K., Ohishi, H., Ohkuma, Y., Ohnishi, T., Ohtake, M., Ogawa, K., Shimbara, Y., Suda, T., Suzuki, S., Takeda, H., Tanaka, K., Watanabe, R., Winkler, M., Yanagisawa, Y., Yasuda, Y., Yoshinaga, K., Yoshida, A., Yoshida, K., Kubo, T., Takechi, M., Ohtsubo, T., Kuboki, T., Fukuda, M., Nishimura, D., Suzuki, T., Yamaguchi, T., Ozawa, A., Moriguchi, T., Sumikama, T., Geissel, H., Aoi, N., Fukuda, N., Hachiuma, I., Inabe, N., Ishibashi, Y., Itoh, Y., Kameda, D., Kusaka, K., Lantz, Mattias, Mihara, M., Miyashita, Y., Momota, S., Namihira, K., Ohishi, H., Ohkuma, Y., Ohnishi, T., Ohtake, M., Ogawa, K., Shimbara, Y., Suda, T., Suzuki, S., Takeda, H., Tanaka, K., Watanabe, R., Winkler, M., Yanagisawa, Y., Yasuda, Y., Yoshinaga, K., Yoshida, A., Yoshida, K., and Kubo, T.

Abstract

Interaction cross sections (σI) for neutron-rich Ne isotopes, 28-32Ne on C target have been measured at 240A MeV using the RIBF at RIKEN. A large enhancement of σI beyond the systematics of stable nuclei have been observed for neutron-rich Ne isotopes, particularly for 31Ne. The possible halo structure for 29,31Ne which would be caused by the lowering of the pf-shell and nuclear deformation of Ne isotopes are discussed by the preliminary analysis.

Published
2010
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22. Reaction cross section studies at NIRS and RIBF

Author

Fukuda, M., Takechi, M., Nishimura, D., Mihara, M., Matsumiya, R., Matsuta, K., Minamisono, T., Ohtsubo, T., Ohkuma, Y., Shimbara, Y., Suzuki, S., Watanabe, R., Izumikawa, T., Momota, S., Suzuki, T., Yamaguchi, T., Kuboki, T., Hachiuma, I., Namihira, K., Nakajima, S., Kobayashi, K., Sumikama, T., Miyashita, Y., Yoshinaga, K., Tanaka, K., Aoi, N., Fukuda, N., Inabe, N., Kameda, D., Kubo, T., Kusaka, K., Lantz, Mattias, Ohnishi, T., Ohtake, M., Suda, T., Takeda, H., Yanagisawa, Y., Yoshida, A., Yoshida, K., Ozawa, A., Moriguchi, T., Ohishi, H., Itoh, Y., Ishibashi, Y., Ogawa, K., Yasuda, Y., Geissel, H., Winkler, M., Sato, S., Kanazawa, M., Kitagawa, A., Fukuda, M., Takechi, M., Nishimura, D., Mihara, M., Matsumiya, R., Matsuta, K., Minamisono, T., Ohtsubo, T., Ohkuma, Y., Shimbara, Y., Suzuki, S., Watanabe, R., Izumikawa, T., Momota, S., Suzuki, T., Yamaguchi, T., Kuboki, T., Hachiuma, I., Namihira, K., Nakajima, S., Kobayashi, K., Sumikama, T., Miyashita, Y., Yoshinaga, K., Tanaka, K., Aoi, N., Fukuda, N., Inabe, N., Kameda, D., Kubo, T., Kusaka, K., Lantz, Mattias, Ohnishi, T., Ohtake, M., Suda, T., Takeda, H., Yanagisawa, Y., Yoshida, A., Yoshida, K., Ozawa, A., Moriguchi, T., Ohishi, H., Itoh, Y., Ishibashi, Y., Ogawa, K., Yasuda, Y., Geissel, H., Winkler, M., Sato, S., Kanazawa, M., and Kitagawa, A.

Abstract

Reaction cross sections for stable nuclei at intermediate energies have been measured precisely and systematically. The data have been found to be reproduced nicely by the optical‐limit approximation of Glauber theory modified to include the nucleon multiple scattering effect and the Fermi‐motion effect. Applying this prescription, the nucleon density distribution of 17Ne has been studied. The surface structure of 8B and 11Be has been also studied using this prescription and hydrogen targets. Using the RIBF that has just started application to studies of exotic nuclei, neutron‐rich Ne isotopes around the Island of Inversion have been investigated through measurements of their interaction cross sections.

Published
2010
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23. Two-step evolution of auroral acceleration at substorm onset

Author

Morioka, A., Miyoshi, Y., Miyashita, Y., Kasaba, Y., Misawa, H., Tsuchiya, F., Kataoka, R., Kadokura, A., Mukai, T., Yumoto, K., Menietti, D.J., Parks, G., Liou, K., Honary, F., Donovan, E., Morioka, A., Miyoshi, Y., Miyashita, Y., Kasaba, Y., Misawa, H., Tsuchiya, F., Kataoka, R., Kadokura, A., Mukai, T., Yumoto, K., Menietti, D.J., Parks, G., Liou, K., Honary, F., and Donovan, E.

Published
2010

24. Search for VHE gamma rays from SS433/W50 with the CANGAROO-II telescope

Author

Hayashi, Sei., Kajino, F., Naito, T., Asahara, A., Bicknell, G. V., Clay, R. W., Doi, Y., Edwards, P. G., Enomoto, R., Gunji, S., Hara, S., Hara, T., Hattori, T., Itoh, C., Kabuki, S., Katagiri, H., Kawachi, A., Kifune, T., Ksenofontov, L. T., Kubo, H., Kurihara, T., Kurosaka, R., Kushida, J., Matsubara, Y., Miyashita, Y., Mizumoto, Y., Mori, M., Mori, H., Muraishi, H., Muraki, Y., Nakase, T., Nishida, D., Nishijima, K., Ohishi, M., Okumura, K., Patterson, J. R., Protheroe, R. J., Sakamoto, N., Sakurazawa, K., Swaby, D. L., Tanimori, T., Tanimura, H., Thornton, G., Tokanai, F., Tsuchiya, K., Uchida, T., Watanabe, S., Yamaoka, T., Yanagita, S., Yoshida, T., Yoshikoshi, T., Hayashi, Sei., Kajino, F., Naito, T., Asahara, A., Bicknell, G. V., Clay, R. W., Doi, Y., Edwards, P. G., Enomoto, R., Gunji, S., Hara, S., Hara, T., Hattori, T., Itoh, C., Kabuki, S., Katagiri, H., Kawachi, A., Kifune, T., Ksenofontov, L. T., Kubo, H., Kurihara, T., Kurosaka, R., Kushida, J., Matsubara, Y., Miyashita, Y., Mizumoto, Y., Mori, M., Mori, H., Muraishi, H., Muraki, Y., Nakase, T., Nishida, D., Nishijima, K., Ohishi, M., Okumura, K., Patterson, J. R., Protheroe, R. J., Sakamoto, N., Sakurazawa, K., Swaby, D. L., Tanimori, T., Tanimura, H., Thornton, G., Tokanai, F., Tsuchiya, K., Uchida, T., Watanabe, S., Yamaoka, T., Yanagita, S., Yoshida, T., and Yoshikoshi, T.

Abstract

SS433, located at the center of the supernova remnant W50, is a close proximity binary system consisting of a compact star and a normal star. Jets of material are directed outwards from the vicinity of the compact star symmetrically to the east and west. Non-thermal hard X-ray emission is detected from lobes lying on both sides. Shock accelerated electrons are expected to generate sub-TeV gamma rays through the inverse-Compton process in the lobes. Observations of the western X-ray lobe region of SS433/W50 system have been performed to detect sub-TeV gamma-rays using the 10m CANGAROO-II telescope in August and September, 2001, and July and September, 2002. The total observation times are 85.2 hours for ON source, and 80.8 hours for OFF source data. No significant excess of sub-TeV gamma rays has been found at 3 regions of the western X-ray lobe of SS433/W50 system. We have derived 99% confidence level upper limits to the fluxes of gamma rays and have set constraints on the strengths of the magnetic fields assuming the synchrotron/inverse-Compton model for the wide energy range of photon spectrum from radio to TeV. The derived lower limits are 4.3 microgauss for the center of the brightest X-ray emission region and 6.3 microgauss for the far end from SS433 in the western X-ray lobe. In addition, we suggest that the spot-like X-ray emission may provide a major contribution to the hardest X-ray spectrum in the lobe., Comment: 7 pages, 8 figures, to be published in Astroparticle Physics

Published
2009
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25. Search for VHE gamma rays from SS433/W50 with the CANGAROO-II telescope

Author

Hayashi, Sei., Kajino, F., Naito, T., Asahara, A., Bicknell, G. V., Clay, R. W., Doi, Y., Edwards, P. G., Enomoto, R., Gunji, S., Hara, S., Hara, T., Hattori, T., Itoh, C., Kabuki, S., Katagiri, H., Kawachi, A., Kifune, T., Ksenofontov, L. T., Kubo, H., Kurihara, T., Kurosaka, R., Kushida, J., Matsubara, Y., Miyashita, Y., Mizumoto, Y., Mori, M., Mori, H., Muraishi, H., Muraki, Y., Nakase, T., Nishida, D., Nishijima, K., Ohishi, M., Okumura, K., Patterson, J. R., Protheroe, R. J., Sakamoto, N., Sakurazawa, K., Swaby, D. L., Tanimori, T., Tanimura, H., Thornton, G., Tokanai, F., Tsuchiya, K., Uchida, T., Watanabe, S., Yamaoka, T., Yanagita, S., Yoshida, T., Yoshikoshi, T., Hayashi, Sei., Kajino, F., Naito, T., Asahara, A., Bicknell, G. V., Clay, R. W., Doi, Y., Edwards, P. G., Enomoto, R., Gunji, S., Hara, S., Hara, T., Hattori, T., Itoh, C., Kabuki, S., Katagiri, H., Kawachi, A., Kifune, T., Ksenofontov, L. T., Kubo, H., Kurihara, T., Kurosaka, R., Kushida, J., Matsubara, Y., Miyashita, Y., Mizumoto, Y., Mori, M., Mori, H., Muraishi, H., Muraki, Y., Nakase, T., Nishida, D., Nishijima, K., Ohishi, M., Okumura, K., Patterson, J. R., Protheroe, R. J., Sakamoto, N., Sakurazawa, K., Swaby, D. L., Tanimori, T., Tanimura, H., Thornton, G., Tokanai, F., Tsuchiya, K., Uchida, T., Watanabe, S., Yamaoka, T., Yanagita, S., Yoshida, T., and Yoshikoshi, T.

Abstract

SS433, located at the center of the supernova remnant W50, is a close proximity binary system consisting of a compact star and a normal star. Jets of material are directed outwards from the vicinity of the compact star symmetrically to the east and west. Non-thermal hard X-ray emission is detected from lobes lying on both sides. Shock accelerated electrons are expected to generate sub-TeV gamma rays through the inverse-Compton process in the lobes. Observations of the western X-ray lobe region of SS433/W50 system have been performed to detect sub-TeV gamma-rays using the 10m CANGAROO-II telescope in August and September, 2001, and July and September, 2002. The total observation times are 85.2 hours for ON source, and 80.8 hours for OFF source data. No significant excess of sub-TeV gamma rays has been found at 3 regions of the western X-ray lobe of SS433/W50 system. We have derived 99% confidence level upper limits to the fluxes of gamma rays and have set constraints on the strengths of the magnetic fields assuming the synchrotron/inverse-Compton model for the wide energy range of photon spectrum from radio to TeV. The derived lower limits are 4.3 microgauss for the center of the brightest X-ray emission region and 6.3 microgauss for the far end from SS433 in the western X-ray lobe. In addition, we suggest that the spot-like X-ray emission may provide a major contribution to the hardest X-ray spectrum in the lobe., Comment: 7 pages, 8 figures, to be published in Astroparticle Physics

Published
2009
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26. Retreat and reformation of X-line during quasi-continuous tailward-of-the-cusp reconnection under northward IMF

Author

Hasegawa, H., Retino, A., Vaivads, Andris, Khotyaintsev, Yuri, Nakamura, R., Takada, T., Miyashita, Y., Reme, H., Lucek, E. A., Hasegawa, H., Retino, A., Vaivads, Andris, Khotyaintsev, Yuri, Nakamura, R., Takada, T., Miyashita, Y., Reme, H., and Lucek, E. A.

Abstract

We present observations on 19-20 November 2006 by the Cluster spacecraft that were skimming the high-latitude dusk-flank magnetopause, which are consistent with more than one reconnection X-line present on the tailward side of the cusp under northward IMF. Evidence of quasi-continuous reconnection over 16 hours exists in the form of Alfvenic acceleration of magnetosheath ions found almost always when either of the satellites traversed the boundary. The data indicate that a dominant X-line was sunward of Cluster for most of the time, but ion velocity distributions consisting of two magnetosheath populations demonstrate that for part of the time, more than one X-line existed. Further, the motion of reconnected field lines shows that some X-line(s) retreated tailward. It is inferred that following the X-line retreat, another X-line reformed sunward of Cluster, leading tomultiple X-lines.

Published
2008
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27. Retreat and reformation of X-line during quasi-continuous tailward-of-the-cusp reconnection under northward IMF

Author

Hasegawa, H., Retino, A., Vaivads, Andris, Khotyaintsev, Yuri, Nakamura, R., Takada, T., Miyashita, Y., Reme, H., Lucek, E. A., Hasegawa, H., Retino, A., Vaivads, Andris, Khotyaintsev, Yuri, Nakamura, R., Takada, T., Miyashita, Y., Reme, H., and Lucek, E. A.

Abstract

We present observations on 19-20 November 2006 by the Cluster spacecraft that were skimming the high-latitude dusk-flank magnetopause, which are consistent with more than one reconnection X-line present on the tailward side of the cusp under northward IMF. Evidence of quasi-continuous reconnection over 16 hours exists in the form of Alfvenic acceleration of magnetosheath ions found almost always when either of the satellites traversed the boundary. The data indicate that a dominant X-line was sunward of Cluster for most of the time, but ion velocity distributions consisting of two magnetosheath populations demonstrate that for part of the time, more than one X-line existed. Further, the motion of reconnected field lines shows that some X-line(s) retreated tailward. It is inferred that following the X-line retreat, another X-line reformed sunward of Cluster, leading tomultiple X-lines., QC 20190624

Published
2008
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28. Detection of Sub-TeV Gamma Rays from the Galactic Center Direction by CANGAROO-II

Author

Tsuchiya, K, Enomoto, R, Ksenofontov, L, Mori, Masaki, Naito, T, Asahara, A, Bicknell, Geoffrey, Clay, Roger W, Doi, Y, Edwards, Philip G, Gunji, S, Hara, Shinji, Hara, T, Hattori, T, Hayashi, Sei, Itoh, Chie, Kabuki, S, Kajino, F, Katagiri, H, Kawachi, A, Kifune, Tadashi, Kubo, H, Kuraeva, T L, Kurosaka, R, Kushida, J, Matsubara, Y, Miyashita, Y, Mizumoto, Y, Moro, H, Muraishi, H, Muraki, Y, Nakase, T, Nishida, D, Nishijima, K, Ohishi, M, Okumura, K, Patterson, Joseph R, Protheroe, Raymond, Sakamoto, N, Sakurazawa, K, Swaby, D L, Tanimori, T, Tanimura, H, Thornton, G J, Tokanai, F, Uchida, T, Watanabe, S, Yamaoka, T, Yanagita, S, Yoshida, T, Yoshikoshi, T, Tsuchiya, K, Enomoto, R, Ksenofontov, L, Mori, Masaki, Naito, T, Asahara, A, Bicknell, Geoffrey, Clay, Roger W, Doi, Y, Edwards, Philip G, Gunji, S, Hara, Shinji, Hara, T, Hattori, T, Hayashi, Sei, Itoh, Chie, Kabuki, S, Kajino, F, Katagiri, H, Kawachi, A, Kifune, Tadashi, Kubo, H, Kuraeva, T L, Kurosaka, R, Kushida, J, Matsubara, Y, Miyashita, Y, Mizumoto, Y, Moro, H, Muraishi, H, Muraki, Y, Nakase, T, Nishida, D, Nishijima, K, Ohishi, M, Okumura, K, Patterson, Joseph R, Protheroe, Raymond, Sakamoto, N, Sakurazawa, K, Swaby, D L, Tanimori, T, Tanimura, H, Thornton, G J, Tokanai, F, Uchida, T, Watanabe, S, Yamaoka, T, Yanagita, S, Yoshida, T, and Yoshikoshi, T

Abstract

We have detected sub-TeV gamma-ray emission from the direction of the Galactic center (GC) using the CANGAROO-II Imaging Atmospheric Cerenkov Telescope. We detected a statistically significant excess at energies greater than 250 GeV. The flux was 1 order

Published
2004

29. Status of the CANGAROO-III project

Author

Kubo, H, Asahara, A, Bicknell, Geoffrey, Clay, Roger W, Doi, Y, Edwards, Philip G, Enomoto, R, Gunji, S, Hara, Shinji, Hara, T, Hattori, T, Hayashi, Sei, Itoh, Chie, Kabuki, S, Kajino, F, Katagiri, H, Kawachi, A, Kifune, Tadashi, Ksenofontov, L, Kuraeva, T L, Kurosaka, R, Kushida, J, Matsubara, Y, Miyashita, Y, Mizumoto, Y, Mori, Masaki, Moro, H, Muraishi, H, Muraki, Y, Naito, T, Nakase, T, Nishida, D, Nishijima, K, Ohishi, M, Okumura, K, Patterson, Joseph R, Protheroe, Raymond, Sakamoto, N, Sakurazawa, K, Swaby, D L, Tanimori, T, Tanimura, H, Thornton, G J, Tokanai, F, Tsuchiya, K, Uchida, T, Watanabe, S, Yamaoka, T, Yanagita, S, Yoshida, T, Yoshikoshi, T, Kubo, H, Asahara, A, Bicknell, Geoffrey, Clay, Roger W, Doi, Y, Edwards, Philip G, Enomoto, R, Gunji, S, Hara, Shinji, Hara, T, Hattori, T, Hayashi, Sei, Itoh, Chie, Kabuki, S, Kajino, F, Katagiri, H, Kawachi, A, Kifune, Tadashi, Ksenofontov, L, Kuraeva, T L, Kurosaka, R, Kushida, J, Matsubara, Y, Miyashita, Y, Mizumoto, Y, Mori, Masaki, Moro, H, Muraishi, H, Muraki, Y, Naito, T, Nakase, T, Nishida, D, Nishijima, K, Ohishi, M, Okumura, K, Patterson, Joseph R, Protheroe, Raymond, Sakamoto, N, Sakurazawa, K, Swaby, D L, Tanimori, T, Tanimura, H, Thornton, G J, Tokanai, F, Tsuchiya, K, Uchida, T, Watanabe, S, Yamaoka, T, Yanagita, S, Yoshida, T, and Yoshikoshi, T

Abstract

The CANGAROO-III project, which consists of an array of four 10-m atmospheric Cherenkov telescopes for gamma-ray astrophysics, started in 1999 in Woomera, South Australia. The first 10-m telescope has been in operation since 2000, and stereoscopic observations with the first and second telescopes started in 2002. The full array will be operational in 2003. Here we report on the status of the CANGAROO-III project including the results of observations with the first telescope.

Published
2004

34. Observation tests on behaviour of nodule gathering mechanism using cutting plate and water jet. Development studies on ocean mining collector system (1).

Author

Handa K., Miyashita Y., Yamakado N., Handa K., Miyashita Y., and Yamakado N.

Abstract

Tests have been conducted on a new mechanism for collecting manganese nodules. The design involves a cutting plate together with a group of water jets and is based on previous studies of dredge buckets. Satisfactory results were obtained in both indoor and shallow water tests, but the design still needs some modification., Tests have been conducted on a new mechanism for collecting manganese nodules. The design involves a cutting plate together with a group of water jets and is based on previous studies of dredge buckets. Satisfactory results were obtained in both indoor and shallow water tests, but the design still needs some modification.

35. Dredging path of buckets on the sea bottom: studies on continuous line bucket mining system for manganese nodules (7).

Author

Handa K., Miyashita Y., Yamakado N., Handa K., Miyashita Y., and Yamakado N.

Abstract

A theoretical analysis of dredging paths is given, and experiments performed with a rope circulation speed slower than the ship speed reported., A theoretical analysis of dredging paths is given, and experiments performed with a rope circulation speed slower than the ship speed reported.

36. Dredging paths of buckets on the sea bottom (part 2). Studies on CLB mining system for manganese nodules (4th report).

Author

Yamakado N., Handa K., Miyashita Y., Yamakado N., Handa K., and Miyashita Y.

Abstract

A theoretical analysis of dredging paths is given, and experiments performed with a rope circulation speed slower than the ship speed reported., A theoretical analysis of dredging paths is given, and experiments performed with a rope circulation speed slower than the ship speed reported.

37. Required rope length and daily production of practical continuous line bucket mining system.

Author

Handa K., Miyashita Y., Yamakado N., Handa K., Miyashita Y., and Yamakado N.

Abstract

Calculations using the previously described discrete parameter method show that manganese nodule production of between 2500 and 2800 t/day may be obtained using 2 m. buckets spaced at 30 m on polyaramid braided rope three to four times as long as the water depth in which the system is to work. A 4000 KW shipboard traction machine is required. Premises and assumptions of the calculations are discussed., Calculations using the previously described discrete parameter method show that manganese nodule production of between 2500 and 2800 t/day may be obtained using 2 m. buckets spaced at 30 m on polyaramid braided rope three to four times as long as the water depth in which the system is to work. A 4000 KW shipboard traction machine is required. Premises and assumptions of the calculations are discussed.

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