Fluxes of Galactic Cosmic Rays

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Cynthia Chandler
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2 n m l k o d ; Fluxes of alactic Cosmic Rays sr s m - ev Flux - solar Modulation: Φ = 550 MV proton helium positron electron antiproton photon ald 50080/60080 (γ) Status of Cosmic Ray Measurements: ood areement beteen cosmic ray propaation/production model and data in backround fluxes (, nuclei) eneral model orks!,, other heay AMS-0 electrons AMS-0 positrons AT 9/5 positrons AMS-0 protons AMS-0 helium MAX antiprotons Caprice 9 antiprotons Caprice 98 antiprotons SS 95/9 antiprotons SS 0 antiprotons kinetic nery [ev] bd d J Z DC[ J C QSRT DC

3 n m l k o p l r o d ; Fluxes of alactic Cosmic Rays sr s m - ev Flux solar Modulation: Φ = 550 MV AMS-0 electrons AMS-0 positrons AT 9/5 positrons AMS-0 protons AMS-0 helium MAX antiprotons Caprice 9 antiprotons Caprice 98 antiprotons SS 95/9 antiprotons SS 0 antiprotons proton helium positron electron antiproton photon kinetic nery [ev] ald 50080/60080 (γ) Status of Cosmic Ray Measurements: ood areement beteen cosmic ray propaation/production model and data in backround fluxes (, nuclei) eneral model orks!,, q k,, other heay are sensitie to dark matter sinals (annihilation) and fluxes/fractions sho some unexplained features need precise measurement of fluxes up to hih eneries! bd d J Z DC[ J C QSRT DC

4 n m l k o p l r o t s d ; Fluxes of alactic Cosmic Rays sr s m - ev Flux solar Modulation: Φ = 550 MV AMS-0 electrons AMS-0 positrons AT 9/5 positrons AMS-0 protons AMS-0 helium MAX antiprotons Caprice 9 antiprotons Caprice 98 antiprotons SS 95/9 antiprotons SS 0 antiprotons proton helium positron electron antiproton photon kinetic nery [ev] ald 50080/60080 (γ) Status of Cosmic Ray Measurements: ood areement beteen cosmic ray propaation/production model and data in backround fluxes (, nuclei) eneral model orks!,, q k,, other heay are sensitie to dark matter sinals (annihilation) and fluxes/fractions sho some unexplained features need precise measurement of fluxes up to hih eneries! alloon xperiment: nestiate influence of atmosphere on flux measurements! bd d J Z DC[ J C QSRT DC

5 T ; Requirements for positron flux measurements electron : antiproton proton : positron 5 solar Modulation: Φ = 550 MV Flux Ratio ald 50080/60080 (γ) kinetic nery [ev] total reection is made up of the sinle reections of the different sutectors bd`d J Z \S] Z DC[ J C QSRT DC

6 bd d u T ; Air shoer in arth s atmosphere J Z \S] Z DC[ J C QSRT DC

7 x y z ; ANTOCOSMCS Simulation of the arth s atmosphere and manetic field ith ANTOCOSMCS (deeloped by. Desorher, Uni. ern laurent/planetocosmics) eneral properties: based on ANT atmospheric model: NRMSS manetic field: RF solar modulation: mean field approximation bd d J Z DC[ J C QSRT DC

8 x y o y z ; ANTOCOSMCS Simulation of the arth s atmosphere and manetic field ith ANTOCOSMCS (deeloped by. Desorher, Uni. ern laurent/planetocosmics) eneral properties: based on ANT atmospheric model: NRMSS manetic field: RF solar modulation: mean field approximation properties of this simulation: input spectra are the fluxes of the conentional alprop model tuned in the loer enery reion to match the data (ald astro-ph/0065) detection planes in seeral altitudes around the earth particle un in km heiht startin positions are choosen to produce a isotropic distribution of cosmic rays only primaries that can hit the detection planes are started bd d J Z DC[ J C QSRT DC

9 f ; Scheme of simulations and analysis ANTOCOSMCS simulate at South ole extract alactic fluxes calculate errors compare secondary muons ith SS Ft. Sumner, TX erify simulation solar Modulation force field approximation isotropic distribution in 0km heiht arth s manetic field and atmosphere (RF, NRMSS00) produce spectra of alactic cosmic ray ARO DarkSUSY bd d J Z DC[ J C QSRT DC

10 Œ l ƒ { l ƒ s Œ x x y x T ; Solar Modulation taken from: Journal of eophysical Research, Vol. : Usoskin et. al., A physical reconstruction of cosmic ray intensity since 6 solar modulated flux, mean field approximation: Ž ƒ S ˆ Š ƒ S S ~} { S MV D : / Ft. Sumner MV y : / South ole bd d J Z \S] Z DC[ J C QSRT DC

11 y bd c d T ; sotropic distribution of cosmic rays km startin plane sin(latitude) lonitude [de] entries [#] entries [#] 5 5 azimuth [de] cos(zenith) J Z \S] Z DC[ J C QSRT DC

12 bd c d T ; sotropic distribution of cosmic rays km detection plane sin(latitude) lonitude [de] entries [#] entries [#] 5 5 azimuth [de] cos(zenith) J Z \S] Z DC[ J C QSRT DC

13 œ s ; NRMSS atmospheric model & depth NRMSS properties: atmospheric model fitted to. data of satellite accelerometers and orbit determination (mass density). data of incoherent scatter radar (temperature). data of solar ultraiolet occulatation (O mass density) dependency on date/solar and manetic parameters dintion of atmospheric depth: œ š d œ altitude dependent atmospheric density, proided by the NASA ia: detection altitude bd d J Z DC[ J C QSRT DC

14 T ; Temperature & depth profile ].5.5 depth [/cm.5 latitude [de] lonitude [de] latitude [de] Depth Temperature Calculations done ith the folloin parameters: km altitude for the solar and manetic parameters : x Ÿž ž date: bd d ea J Z \S] Z C[ J C Q RT C temperature [K] 0 lonitude [de]

15 s y s t s a a ; Depth oer time on South ole ] depth [/cm year [a] km altitude latitude de, lonitude solar and manetic parameters for each day de: mean traectory on South ole time has the larest influence on the atmospheric depth (only small dependency on solar and manetic parameters) bd d J Z C[ J C Q RT C

16 y T ; ) roperties of arth s Atmosphere (NRMSS de), de, lon.: Calculation at mean balloon traectory at south pole (lat.: x y Dec Temperature [de Celsius] Altitude [km] kinetic enery/temperature of atmosphere (ideal as) bd da d J Z \S] Z C[ J C Q RT C

17 a ; Mean radiation lenth in Dec. at the South ole entries [#] number of radiation lenths calculated ith the atmospheric model and the traectory of the cosmic rays mean number of crossed radiation lenths of all cosmic rays bore % because of the anular distribution of cosmic rays km is bd`d J Z C[ J C Q RT C

18 bd d u a T ; Riidity Cutoff ith RF J Z \S] Z C[ J C Q RT C

19 x bd d z a T ; Verification of atmospheric physics model 000 m,. /cm sr s m - ] 0000 m, /cm Flux [ev SS. /cm SS.68 /cm - nery [ev] ). / Comparison of simulations ith SS data in Ft. Sumner, TX ( Simulation seems to ork ithin the errors! J Z \S] Z C[ J C Q RT C

20 f a ; ositron fluxes in km South ole Dec. sr s m - ] Flux [ev primary enerated, D total, 0000 m, D primary, 0000 m, D secondary, 0000 m, D Ratio total, 0000 m, D primary en. primary, 0000 m, D primary en nery [ev] - nery [ev] simulations done in the same ay as for Ft. Sumner, except of date and location bd d J Z C[ J C Q RT C

21 ««s «º s ¹ ««a ; ositron fluxes in km corrections S prim S atmo meanin of quantities: sec S tot ª tot (all quantities are enery dependent) S number of particles (alrop, ANTOCOSMCS): S,, sec,, tot tot prim detection ficiency (detector simulation): to take loer acceptance of TRD into account: S y ž ev ³² ± p proton Reection (detector simulation):» s ª for all eneries ev p m a µ loss of particles in atmosphere (ANTOCOSMCS): atmo enery dependent tracker misidentification (detector simulation): S enery dependent bd d J Z C[ J C Q RT C

22 ««s «º s ¹ ««¼ y a ; ositron fluxes in km corrections S prim S atmo meanin of quantities: sec S tot ª tot (all quantities are enery dependent) S number of particles (alrop, ANTOCOSMCS): S,, sec,, tot tot prim detection ficiency (detector simulation): to take loer acceptance of TRD into account: S y ž ev ³² ± p proton Reection (detector simulation):» s ª for all eneries ev p m a µ loss of particles in atmosphere (ANTOCOSMCS): atmo enery dependent tracker misidentification (detector simulation): S enery dependent error estimates: statistical errors: systematic errors for atmospheric physics: systematic errors for detector properties: % % bd d J Z C[ J C Q RT C

23 ¾ ½ l p l bd ca d T ; m) S -fluxes ( - and ½ Total counts of 6 [#], S, 0 days, S, 0 days + - total e total e S N 5 nery [ev] counts ith detector ficiencies and atmospheric loss! sr m Ÿž days S ith acceptance J Z \S] Z C[ J C Q RT C

24 bd d a T ; days S lectron and ositron fluxes ith ] 9 Counts [ev 8 sr s m - ] 6 Flux [ev 5 e, S, 0 days e -, S, 0 days con. alprop + AMS-0 electrons AMS-0 positrons AT 9/5 positrons nery [ev] all corrections applied J Z \S] Z C[ J C Q RT C

25 p m l l t s a ; lectron and ositron fluxes ith days S sr s m - ] Flux [ev AMS-0 electrons AMS-0 positrons AT 9/5 positrons + e, S, 0 days - e, S, 0 days con. alprop nery [ev] ] Counts [ev - e + e + +e ositron Fraction - S, 0 days AT AMS0 con. alprop nery [ev] all corrections applied assumptions for and same behaiour in atmosphere same reection same tracker resolution smaller errors ( atmo cancels in fraction) : bd d J Z C[ J C Q RT C

26 a ; lectron and ositron fluxes ith days S sr s m - ] Flux [ev AMS-0 electrons AMS-0 positrons AT 9/5 positrons + e, S, 0 days - e, S, 0 days con. alprop nery [ev] ] Counts [ev - e + e + +e ositron Fraction - S, 0 days AT AMS0 con. alprop nery [ev] all corrections applied S errors are dominated by statistics at hiher eneries this S has ca. AT ÁÀ statistics of bd d J Z C[ J C Q RT C

27 a ; lectron and ositron fluxes ith days S sr s m - ] Flux [ev AMS-0 electrons AMS-0 positrons AT 9/5 positrons + e, S, 0 days - e, S, 0 days con. alprop nery [ev] ] Counts [ev - e + e + +e ositron Fraction - m / = 500 ev, m = 00 ev 0 tanβ= 5, µ>0, A = 0 0 DM sinal boost factor: 5.0 S, 0 days AT AMS0 alprop + DM DM, DarkSUSY con. alprop nery [ev] all corrections applied this dark matter sinal is probably distinuishable ith a fliht in km altitude days S bd d J Z C[ J C Q RT C

28 ed ; Antiproton fluxes in km (counts for days ith acceptance ž m sr and ithout detector fiencies) sr s m - ] Flux [ev primary enerated, D total, 0000 m, D primary, 0000 m, D secondary, 0000 m, D nery [ev] influence of atmosphere seems to be in the same order as for positrons! bd d J Z C[ J C Q RT C

29 Â l t s ed ; Antiproton fluxes in km (counts for days ith acceptance ž m sr and ithout detector fiencies) sr s m - ] Flux [ev primary enerated, D total, 0000 m, D primary, 0000 m, D secondary, 0000 m, D ] + Antiproton Fraction [p/p - - MAX Caprice 98 Caprice 9 SS 95/9 SS 0 eat S, 0 days con. alprop -6 - nery [ev] -5 nery [ev] influence of atmosphere seems to be in the same order as for positrons! same assumptions for detector ficiencies as for room for improement! bd d J Z C[ J C Q RT C

30 ed ; Antiproton fluxes in km (counts for days ith acceptance ž m sr and ithout detector fiencies) sr s m - ] Flux [ev primary enerated, D total, 0000 m, D primary, 0000 m, D secondary, 0000 m, D ] + Antiproton Fraction [p/p - - m / = 500 ev, m = 00 ev 0 tanβ= 5, µ>0, A = 0 0 DM sinal boost factor:.0 MAX Caprice 98 Caprice 9 SS 95/9 SS 0 eat S, 0 days alprop + DM DM, DarkSUSY con. alprop -6 - nery [ev] -5 nery [ev] influence of atmosphere seems to be in the same order as for positrons! dark matter contribution bd d J Z C[ J C Q RT C

31 r a d ; hoton fluxes in km (counts for days ith acceptance ž m sr and ithout detector fiencies) sr s m - ] Flux [ev primary enerated, D total, 0000 m, D primary, 0000 m, D secondary, 0000 m, D nery [ev] diffuse s, aeraed oer all directions in the alaxy bd d J Z C[ J C Q RT C

32 r T ; km hoton fluxes in sr and ithout detector fiencies) m ž days ith acceptance (counts for s, aeraed oer all directions in the alaxy diffuse too many secondaries, flux measurement not possible! bd ad d J Z \S] Z C[ J C Q RT C

33 Ã Å Ä Ã Ã Ç K Å Æ Ã d d ; Summary & Outlook What hae been done: simulation of the positron fraction measurement on the South ole in km altitude ith S error estimation includin the correction of the main uncertainties ood measurement of positron fraction possible (ca. statistics of AT) ood measurement of antiproton ratio possible bd d J Z C[ J C Q RT C

34 Ã Å Ä Ã Ã Ç K Å Æ Ã Ã Ã Ã Ã d d ; Summary & Outlook What hae been done: simulation of the positron fraction measurement on the South ole in km altitude ith S error estimation includin the correction of the main uncertainties ood measurement of positron fraction possible (ca. statistics of AT) ood measurement of antiproton ratio possible What should be done: use more precise properties of S detector find a better implementation of hih eneretic alphas find out about the detecabilty of heay ions to measure e.. /C ratio check for detectibility of other dark matter sinals bd d J Z C[ J C Q RT C

Fluxes of Galactic Cosmic Rays

Fluxes of Galactic Cosmic Rays o n m l p Flues o alactic Cosmic Rays sr s m - ev Flu - solar Modulation: Φ = 550 MV proton helium positron electron antiproton photon galde 50080/60080 (γ) Status o Cosmic Ray Measurements: good agreement