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Galactic Cosmic Ray Energy Spectra for Heavy Elements (Ne to Zn) from ∼0.8 to ∼10 GeV/nuc with the SuperTIGER Instrument

Labrador, A. W. and Binns, W. R. and Rose, R. G. and Brandt, T. J. and Dowkontt, P. F. and Hams, T. and Israel, M. H. and Link, J. T. and Mewaldt, R. A. and Mitchell, J. W. and Murphy, R. P. and Rauch, B. F. and Sakai, K. and Sasaki, M. and Stone, E. C. and Waddington, C. J. and Walsh, N. E. and Ward, J. E. and Wiedenbeck, M. E. (2019) Galactic Cosmic Ray Energy Spectra for Heavy Elements (Ne to Zn) from ∼0.8 to ∼10 GeV/nuc with the SuperTIGER Instrument. In: 36th International Cosmic Ray Conference (ICRC2019). Proceedings of Science. No.358. SISSA , Trieste, Italy, Art. No. 95. https://resolver.caltech.edu/CaltechAUTHORS:20190821-073116292

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Abstract

SuperTIGER (Trans-Iron Galactic Element Recorder) is a large-area balloon-borne instrument built to measure the galactic cosmic-ray (GCR) abundances of elements from Z=10 (Ne) through Z=56 (Ba) at energies from ~0.8 to ~10 GeV/nuc. SuperTIGER flew over Antarctica for a record-breaking 55 days, from December 8, 2012 to February 1, 2013. We will report progress on calculations of galactic cosmic ray spectra corrected to the top of the atmosphere for abundant elements between Ne and Zn from the SuperTIGER flight data. The energy spectra calculations will include up to date refinements to the energy calibrations for the acrylic and aerogel Cherenkov detectors in the instrument, and we will report on new instrument and atmospheric corrections to the top of the atmosphere for energies and abundances. Heinz and Sunyaev (2002) suggested that microquasar jets like those observed in GRS 1915+105 and GRO J1655-40 may be observable as near monoenergetic peaks in heavy ion spectra in the 3-10 GeV/nuc energy range. The large area and long flight duration of SuperTIGER is particularly suited to looking for these microquasar signatures with good statistics. We will compare our SuperTIGER spectra with ACE/CRIS and HEAO-3 spectra and with model GCR spectra solar modulated for the time period of the flight, and we will search for features that may be produced by microquasar jets.


Item Type:Book Section
Related URLs:
URLURL TypeDescription
https://pos.sissa.it/358/095/PublisherArticle
ORCID:
AuthorORCID
Labrador, A. W.0000-0001-9178-5349
Binns, W. R.0000-0001-6110-3407
Brandt, T. J.0000-0003-4087-1786
Israel, M. H.0000-0002-8104-208X
Mewaldt, R. A.0000-0003-2178-9111
Stone, E. C.0000-0002-2010-5462
Wiedenbeck, M. E.0000-0002-2825-3128
Additional Information:© 2019 owned by the author(s) under the term of the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License. Pre-published on: 2019 July 22. This work was supported by NASA under grants NNX09AC17G, NNX09AC18G, NNX14AB24G, NNX14AB25G, and NNX15AC15G, by the Peggy and Steve Fossett Foundation, and by the McDonnell Center for the Space Sciences at Washington University in St. Louis. We thank the ACE/CRIS instrument team and the ACE Science Center for providing ACE data.
Group:Space Radiation Laboratory
Funders:
Funding AgencyGrant Number
NASANNX09AC17G
NASANNX09AC18G
NASANNX14AB24G
NASANNX14AB25G
NASANNX15AC15G
Peggy and Steve Fossett FoundationUNSPECIFIED
Washington UniversityUNSPECIFIED
Series Name:Proceedings of Science
Issue or Number:358
Record Number:CaltechAUTHORS:20190821-073116292
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20190821-073116292
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:98057
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:21 Aug 2019 18:44
Last Modified:20 Feb 2020 14:33

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