Determination of the proton-to-helium ratio in cosmic rays at ultra-high energies from the tail of the X-max distribution

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F68378271%3A_____%2F16%3A00539915" target="_blank" >RIV/68378271:_____/16:00539915 - isvavai.cz</a>

Výsledek na webu

<a href="https://doi.org/10.1016/j.astropartphys.2016.09.007" target="_blank" >https://doi.org/10.1016/j.astropartphys.2016.09.007</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1016/j.astropartphys.2016.09.007" target="_blank" >10.1016/j.astropartphys.2016.09.007</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Determination of the proton-to-helium ratio in cosmic rays at ultra-high energies from the tail of the X-max distribution

Popis výsledku v původním jazyce

We present a method to determine the proton-to-helium ratio in cosmic rays at ultra-high energies. It makes use of the exponential slope, A, of the tail of the X-max. distribution measured by an air shower experiment. The method is quite robust with respect to uncertainties from modeling hadronic interactions and to systematic errors on X-max and energy, and to the possible presence of primary nuclei heavier than helium. Obtaining the proton-to-helium ratio with air shower experiments would be a remarkable achievement. To quantify the applicability of a particular mass-sensitive variable for mass composition analysis despite hadronic uncertainties we introduce as a metric the 'analysis indicator' and find an improved performance of the A method compared to other variables currently used in the literature. The fraction of events in the tail of the Xmax distribution can provide additional information on the presence of nuclei heavier than helium in the primary beam.n

Název v anglickém jazyce

Determination of the proton-to-helium ratio in cosmic rays at ultra-high energies from the tail of the X-max distribution

Popis výsledku anglicky

We present a method to determine the proton-to-helium ratio in cosmic rays at ultra-high energies. It makes use of the exponential slope, A, of the tail of the X-max. distribution measured by an air shower experiment. The method is quite robust with respect to uncertainties from modeling hadronic interactions and to systematic errors on X-max and energy, and to the possible presence of primary nuclei heavier than helium. Obtaining the proton-to-helium ratio with air shower experiments would be a remarkable achievement. To quantify the applicability of a particular mass-sensitive variable for mass composition analysis despite hadronic uncertainties we introduce as a metric the 'analysis indicator' and find an improved performance of the A method compared to other variables currently used in the literature. The fraction of events in the tail of the Xmax distribution can provide additional information on the presence of nuclei heavier than helium in the primary beam.n

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10303 - Particles and field physics

Projekt

—

Návaznosti

—

Rok uplatnění

2016

Kód důvěrnosti údajů

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Název periodika

Astroparticle Physics

ISSN

0927-6505

e-ISSN

—

Svazek periodika

85

Číslo periodika v rámci svazku

Dec

Stát vydavatele periodika

NL - Nizozemsko

Počet stran výsledku

6

Strana od-do

29-34

Kód UT WoS článku

000389112800003

EID výsledku v databázi Scopus

2-s2.0-84995588007