Remember Me
Or use your Academic/Social account:


You have just completed your registration at OpenAire.

Before you can login to the site, you will need to activate your account. An e-mail will be sent to you with the proper instructions.


Please note that this site is currently undergoing Beta testing.
Any new content you create is not guaranteed to be present to the final version of the site upon release.

Thank you for your patience,
OpenAire Dev Team.

Close This Message


Verify Password:
Verify E-mail:
*All Fields Are Required.
Please Verify You Are Human:

OpenAIRE is about to release its new face with lots of new content and services.
During September, you may notice downtime in services, while some functionalities (e.g. user registration, login, validation, claiming) will be temporarily disabled.
We apologize for the inconvenience, please stay tuned!
For further information please contact helpdesk[at]openaire.eu

fbtwitterlinkedinvimeoflicker grey 14rssslideshare1
Kuhar, Matej; Krucker, Säm; Hannah, Iain G.; Glesener, Lindsay; Saint-Hilaire, Pascal; Grefenstette, Brian W.; Hudson, Hugh S.; White, Stephen M.; Smith, David M.; Marsh, Andrew J.; Wright, Paul J.; Boggs, Steven E.; Christensen, Finn Erland; Craig, William W.; Hailey, Charles J.; Harrison, Fiona A.; Stern, Daniel; Zhang, William W. (2017)
Publisher: Institute of Physics Publishing, Inc.
Languages: English
Types: Article
Subjects: Astrophysics - Solar and Stellar Astrophysics, QB, QC, Gamma rays, X-rays [Sun], Solar flares, particle emission [Sun], Astrophysics - High Energy Astrophysical Phenomena
We present observations of the occulted active region AR 12222 during the third Nuclear Spectroscopic Telescope ARray (NuSTAR) solar campaign on 2014 December 11, with concurrent Solar Dynamics Observatory (SDO)/AIA and FOXSI-2 sounding rocket observations. The active region produced a medium-size solar flare 1 day before the observations, at ∼18 UT on 2014 December 10, with the post-flare loops still visible at the time of NuSTAR observations. The time evolution of the source emission in the SDO/AIA 335 Å channel reveals the characteristics of an extreme-ultraviolet late-phase event, caused by the continuous formation of new post-flare loops that arch higher and higher in the solar corona. The spectral fitting of NuSTAR observations yields an isothermal source, with temperature 3.8–4.6 MK, emission measure (0.3–1.8) × 1046 cm−3, and density estimated at (2.5–6.0) × 108 cm−3. The observed AIA fluxes are consistent with the derived NuSTAR temperature range, favoring temperature values in the range of 4.0–4.3 MK. By examining the post-flare loops’ cooling times and energy content, we estimate that at least 12 sets of post-flare loops were formed and subsequently cooled between the onset of the flare and NuSTAR observations, with their total thermal energy content an order of magnitude larger than the energy content at flare peak time. This indicates that the standard approach of using only the flare peak time to derive the total thermal energy content of a flare can lead to a large underestimation of its value.
  • The results below are discovered through our pilot algorithms. Let us know how we are doing!

    • Boerner, P. F., Testa, P., Warren, H., Weber, M. A., & Schrijver, C. J. 2014, Sol. Phys., 289, 2377
    • Cargill, P. J., Mariska, J. T., & Antiochos, S. K. 1995, ApJ, 439, 1034
    • Del Zanna, G. 2013, A&A, 558, A73
    • Dere, K. P., Landi, E., Mason, H. E., Monsignori Fossi, B. C., & Young, P. R. 1997, A&AS, 125
    • Emslie, A. G., Dennis, B. R., Shih, A. Y., et al. 2012, ApJ, 759, 71
    • Fa´rn´ık, F., Sˇvestka, Z., Hudson, H. S., & Uchida, Y. 1996, Sol. Phys., 168, 331
    • Forbes, T. G., & Lin, J. 2000, Journal of Atmospheric and Solar-Terrestrial Physics, 62, 1499
    • Gallagher, P. T., Dennis, B. R., Krucker, S., Schwartz, R. A., & Tolbert, A. K. 2002, Sol. Phys., 210, 341
    • Grefenstette, B. W., Glesener, L., Krucker, S., et al. 2016, ApJ, 826, 20
    • Hannah, I. G., Christe, S., Krucker, S., et al. 2008, ApJ, 677, 704
    • Hannah, I. G., Grefenstette, B. W., Smith, D. M., et al. 2016, ApJ, 820, L14
    • Harrison, F. A., Craig, W. W., Christensen, F. E., et al. 2013, ApJ, 770, 103
    • Howard, T. A., & Harrison, R. A. 2004, Sol. Phys., 219, 315
    • Hudson, H. S., Lemen, J. R., St. Cyr, O. C., Sterling, A. C., & Webb, D. F. 1998, Geophys. Res. Lett., 25, 2481
    • Kopp, R. A., & Poletto, G. 1984, Sol. Phys., 93, 351
    • Krucker, S., Christe, S., Glesener, L., et al. 2014, ApJ, 793, L32
    • Landi, E., Young, P. R., Dere, K. P., Del Zanna, G., & Mason, H. E. 2013, ApJ, 763, 86
    • Lin, R. P., Dennis, B. R., Hurford, G. J., et al. 2002, Sol. Phys., 210, 3
    • Liu, K., Zhang, J., Wang, Y., & Cheng, X. 2013, ApJ, 768, 150
    • MacCombie, W. J., & Rust, D. M. 1979, Sol. Phys., 61, 69
    • Madsen, K. K., Harrison, F. A., Markwardt, C. B., et al. 2015, ApJS, 220, 8
    • McIntosh, S. W., Leamon, R. J., Davey, A. R., & Wills-Davey, M. J. 2007, ApJ, 660, 1653
    • Nitta, N. V., Aschwanden, M. J., Boerner, P. F., et al. 2013, Sol. Phys., 288, 241
    • Parenti, S., Reale, F., & Reeves, K. K. 2010, A&A, 517, A41
    • Reale, F., Guarrasi, M., Testa, P., et al. 2011, ApJ, 736, L16
    • Rust, D. M., & Hildner, E. 1976, Sol. Phys., 48, 381
    • Stewart, R. T., McCabe, M. K., Koomen, M. J., Hansen, R. T., & Dulk, G. A. 1974, Sol. Phys., 36, 203
    • Testa, P., & Reale, F. 2012, ApJ, 750, L10
    • Sˇvestka, Z. 1984, Sol. Phys., 94, 171
    • Sˇvestka, Z., Dennis, B. R., Woodgate, B. E., et al. 1982, Sol. Phys., 80, 143
    • Sˇvestka, Z., Fa´rn´ık, F., Hudson, H. S., et al. 1995, Sol. Phys., 161, 331
    • Warren, H. P., Winebarger, A. R., & Brooks, D. H. 2012, ApJ, 759, 141
    • West, M. J., & Seaton, D. B. 2015, ApJ, 801, L6
    • Withbroe, G. L. 1988, ApJ, 325, 442
    • Woods, T. N. 2014, Sol. Phys., 289, 3391
    • Woods, T. N., Hock, R., Eparvier, F., et al. 2011, ApJ, 739, 59
    • Zarro, D. M., Sterling, A. C., Thompson, B. J., Hudson, H. S., & Nitta, N. 1999, ApJ, 520, L139
  • No related research data.
  • No similar publications.
Cookies make it easier for us to provide you with our services. With the usage of our services you permit us to use cookies.
More information Ok