عنوان

SuperTiger Elemental Abundances for the Charge Range...

Number

TLpq2445909487

.Language of Text, Soundtrack etc

انگلیسی

Title Proper

SuperTiger Elemental Abundances for the Charge Range...

General Material Designation

[Thesis]

First Statement of Responsibility

Walsh, Nathan Elliot

Subsequent Statement of Responsibility

Israel, Martin H

Name of Publisher, Distributor, etc.

Washington University in St. Louis

Date of Publication, Distribution, etc.

2020

Specific Material Designation and Extent of Item

185

Dissertation or thesis details and type of degree

Ph.D.

Body granting the degree

Washington University in St. Louis

Text preceding or following the note

2020

Text of Note

On December 8, 2012 the SuperTIGER (Super Trans-Iron Galactic Element Recorder) instrument was launched from Williams Field, Antarctica on a long-duration balloon flight that lasted 55 days and maintained a mean altitude of 125,000 feet. SuperTIGER measured the relative abundances of Galactic cosmic-ray (GCR) nuclei with high statistical precision and well resolved individual element peaks from usd_usdNe to usd_{40}usdZr. SuperTIGER also made exploratory measurements of the relative abundances up to usd_{56}usdBa. The SuperTIGER instrument determines the charge (usdZusd) and energy of GCR using two independent detector stacks composed of a scintillating fiber hodoscope, two Cherenkov light detectors and three scintillation light detectors. The SuperTIGER data is analyzed to account for instrument effects and then corrected for nuclear interactions and energy losses that occur within the instrument, atmosphere and interstellar medium to obtain relative abundances at the GCR source. The SuperTIGER data analysis reported in Murphy et al. 2016\cite{Murphyetal:2016} was performed prior to the Antarctic recovery effort in 2015 and only included data transmitted during line-of-site periods and via satellite telemetry. The current analysis includes additional data saved to on-board solid-state drives that were retrieved during recovery. Although the statistics are low for elements heavier than usd_{40}usdZr, we show relative abundances of charges usd41\leq Z\leq56usd with individual element resolution. The relative abundances of elements usd_{40}usdZr through usd_{60}usdNd are of particular interest because they are likely formed both by supernova explosions and binary neutron star mergers. A well resolved measurement of this charge range can constrain the contributions to the GCR composition from both these possible sources. The GCR relative elemental abundances derived in this thesis are compared to satellite measurements after accounting for the effects of traversing the instrument and atmosphere. Further work is required to accurately constrain the GCR source composition up to usd_{56}usdBa.

Astrophysics

Cosmic rays

Neutron stars

Physics

Supernovae

Israel, Martin H

Walsh, Nathan Elliot

Electronic name

p

[Thesis]

276903

a

Y