Download - G Kornakov Ea Smultivariate Analysis
![Page 1: G Kornakov Ea Smultivariate Analysis](https://reader033.vdocuments.us/reader033/viewer/2022052619/556da238d8b42a875d8b46d6/html5/thumbnails/1.jpg)
Detecting EAS with TRASGOs-a simulation-
G. Kornakov
February, 2010, Santiago de Compostela
![Page 2: G Kornakov Ea Smultivariate Analysis](https://reader033.vdocuments.us/reader033/viewer/2022052619/556da238d8b42a875d8b46d6/html5/thumbnails/2.jpg)
Extensive air shower (EAS)
● How does an EAS occur? -High energy primary cosmic rays interact at the high atmosphere with production of billions of secondaries and shower formation
● Why are they interesting?-Astroparticle Physics:
– Where do they come from?
– How are they accelerated?
– How do they propagate?
– and many other...
-very high energy (up to 102 0 eV), -understanding of formation process
![Page 3: G Kornakov Ea Smultivariate Analysis](https://reader033.vdocuments.us/reader033/viewer/2022052619/556da238d8b42a875d8b46d6/html5/thumbnails/3.jpg)
The knee region
Knee
1 Partícle/m2-y
1 Partícle/km2-y
1 Partícle/km2-y
![Page 4: G Kornakov Ea Smultivariate Analysis](https://reader033.vdocuments.us/reader033/viewer/2022052619/556da238d8b42a875d8b46d6/html5/thumbnails/4.jpg)
EAS statistics in knee region
The scatter plot of the average logarithm of the nuclear mass number of the primary cosmic rays versus energy clearly shows the need for more input from accelerators.
[CCOU02]
Mass of the primary cosmic ray vs energy measured in different experiments
![Page 5: G Kornakov Ea Smultivariate Analysis](https://reader033.vdocuments.us/reader033/viewer/2022052619/556da238d8b42a875d8b46d6/html5/thumbnails/5.jpg)
EAS simulation
Code: AIRES
Simulations characteristics:
-energy: 101 5 eV (Knee region) -primary particles: P,C,Fe,Gammas
-depth of first interaction:30g/cm2
-number of simulations: 100 for each case.-height of measurement plane: 1400 m
Extensive showers detection on Earth surface
![Page 6: G Kornakov Ea Smultivariate Analysis](https://reader033.vdocuments.us/reader033/viewer/2022052619/556da238d8b42a875d8b46d6/html5/thumbnails/6.jpg)
Variables simulated
● x,y,● θ,φ● time of arrival● energy● height of production
of secondary part.● id. of the secondary
particle
EAS simulation
![Page 7: G Kornakov Ea Smultivariate Analysis](https://reader033.vdocuments.us/reader033/viewer/2022052619/556da238d8b42a875d8b46d6/html5/thumbnails/7.jpg)
EAS simulation
e μ
Some results
![Page 8: G Kornakov Ea Smultivariate Analysis](https://reader033.vdocuments.us/reader033/viewer/2022052619/556da238d8b42a875d8b46d6/html5/thumbnails/8.jpg)
EAS simulationSome results
e μ
Difference between azimuthal angles of electrons and muons vs time φφ
time
time
![Page 9: G Kornakov Ea Smultivariate Analysis](https://reader033.vdocuments.us/reader033/viewer/2022052619/556da238d8b42a875d8b46d6/html5/thumbnails/9.jpg)
e μ
time
θ
time
r
r
θ
EAS simulationSome results
![Page 10: G Kornakov Ea Smultivariate Analysis](https://reader033.vdocuments.us/reader033/viewer/2022052619/556da238d8b42a875d8b46d6/html5/thumbnails/10.jpg)
Lateral distribution in a EAS induced by proton
Lateral distribution of μ+e at different primary energies
~30m
~90m~200m
![Page 11: G Kornakov Ea Smultivariate Analysis](https://reader033.vdocuments.us/reader033/viewer/2022052619/556da238d8b42a875d8b46d6/html5/thumbnails/11.jpg)
R=5particles/m2
R~30m for 101 5ev proton
110
8
6
12
11
9 7
13
3
2
5
4
R
We have started to analyse the answer of a single detector at different distances from the shower core:We assumed S=1m2 detectors
EAS simulation
![Page 12: G Kornakov Ea Smultivariate Analysis](https://reader033.vdocuments.us/reader033/viewer/2022052619/556da238d8b42a875d8b46d6/html5/thumbnails/12.jpg)
RESULTS (time of arrival)
Iron
Carbon
0m R/2~15 m R ~30m
![Page 13: G Kornakov Ea Smultivariate Analysis](https://reader033.vdocuments.us/reader033/viewer/2022052619/556da238d8b42a875d8b46d6/html5/thumbnails/13.jpg)
0m R/2~15 m R ~30m
Proton
Gamma
RESULTS (time of arrival)
![Page 14: G Kornakov Ea Smultivariate Analysis](https://reader033.vdocuments.us/reader033/viewer/2022052619/556da238d8b42a875d8b46d6/html5/thumbnails/14.jpg)
RESULTS (zenithal angle)
0m R/2~15 m R ~30m
Iron
Carbon
![Page 15: G Kornakov Ea Smultivariate Analysis](https://reader033.vdocuments.us/reader033/viewer/2022052619/556da238d8b42a875d8b46d6/html5/thumbnails/15.jpg)
0m R/2~15 m R ~30m
Proton
Gamma
RESULTS (zenithal angle)
![Page 16: G Kornakov Ea Smultivariate Analysis](https://reader033.vdocuments.us/reader033/viewer/2022052619/556da238d8b42a875d8b46d6/html5/thumbnails/16.jpg)
RESULTS (Azimuthal angle in one detector)
Proton Gamma
Iron Carbon
![Page 17: G Kornakov Ea Smultivariate Analysis](https://reader033.vdocuments.us/reader033/viewer/2022052619/556da238d8b42a875d8b46d6/html5/thumbnails/17.jpg)
NEXT STEPS
![Page 18: G Kornakov Ea Smultivariate Analysis](https://reader033.vdocuments.us/reader033/viewer/2022052619/556da238d8b42a875d8b46d6/html5/thumbnails/18.jpg)
To define some secondary observables
● Number of particles <N>, <Ne>,<Nμ>● Arrival Times: <T><Te><Tμ>● Th <Th> and σ(Th) for e and μ at t=5ns,
t=10ns, t=20ns.● <Ph> and σ(Ph) as a function of position
Analyse their behaviour, their correlations, their
clusters...
![Page 19: G Kornakov Ea Smultivariate Analysis](https://reader033.vdocuments.us/reader033/viewer/2022052619/556da238d8b42a875d8b46d6/html5/thumbnails/19.jpg)
One dream
![Page 20: G Kornakov Ea Smultivariate Analysis](https://reader033.vdocuments.us/reader033/viewer/2022052619/556da238d8b42a875d8b46d6/html5/thumbnails/20.jpg)
Why multivariate analysis?
● A lot of information spread out in many observable variables (many dimensions problem)
● Some variables are strongly correlated and dependent on the primary cosmic ray characteristics (energy, mass, direction)
● Many multivariate techniques developed recently and not yet commonly used in astroparticle physics: clusters analysis, PAC analysis …
Problems we expect:● High fluctuations in different EAS from the same primary● High statistical fluctuations inside a single shower
Hope:● To find some hidden relationship among all the observables informing
us about the properties of the primitive cosmic ray
![Page 21: G Kornakov Ea Smultivariate Analysis](https://reader033.vdocuments.us/reader033/viewer/2022052619/556da238d8b42a875d8b46d6/html5/thumbnails/21.jpg)
Still a lot of work
![Page 22: G Kornakov Ea Smultivariate Analysis](https://reader033.vdocuments.us/reader033/viewer/2022052619/556da238d8b42a875d8b46d6/html5/thumbnails/22.jpg)
Acknowledgments
especially want to thank R.Vázquez for his help with the simulations