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ZHAireS and neutrino radio detection Washington Rodrigues de Carvalho Jr. Universidade de Santiago de Compostela carvajr@gmail.com GRAND Workshop, LPNHE, Paris February 9th 2015 February 9th 2015 Washington Carvalho (USC) ZHAireS and

slide-1
SLIDE 1

ZHAireS and neutrino radio detection

Washington Rodrigues de Carvalho Jr.

Universidade de Santiago de Compostela carvajr@gmail.com

GRAND Workshop, LPNHE, Paris February 9th 2015

Washington Carvalho (USC) ZHAireS and neutrino radio detection February 9th 2015 1 / 36

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SLIDE 2

Overview

1

ZHAireS and ZHAireS-Reflex Emission Mechanisms The ZHAireS code Polarization and the Cherenkov ring Some comparisons with data The Two-component approach approximation ZHAireS-Reflex

2

Radio array sensitivity to Earth-Skimming ντ End to end simulation Efficiency and Exposure Sensitivity of a radio array

Washington Carvalho (USC) ZHAireS and neutrino radio detection February 9th 2015 2 / 36

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SLIDE 3

ZHAireS and ZHAireS-Reflex Emission Mechanisms

Emission mechanisms

Two main emission mechanisms:

Geomagnetic emission mechanism Askaryan or charge excess emission mechanism

Moving charged particles radiate Movement can be described in terms of a current J(t) From Lienard-Wiechert potentials (disregarding static term):

  • E ∝ ∂

A ∂t ∝ ∂ J⊥ ∂t , where

  • J⊥ = −ˆ

n × (ˆ n × J) and ˆ n is the observation direction

Antenna J n ^ J

Washington Carvalho (USC) ZHAireS and neutrino radio detection February 9th 2015 3 / 36

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SLIDE 4

ZHAireS and ZHAireS-Reflex Emission Mechanisms

Askaryan Mechanism

Dominates emission in dense media Electron and positron currents are opposite

e+ e- v v J- J+ J+ + J- = 0

  • v approx. paralell to shower axis

Emission is due to an excess of electrons in the shower

Shower front entrains electrons from medium

(Compton, Møller, Bhabba and positron anihilation)

G.A. Askaryan, Soviet JETP 21 (1965) 658

Washington Carvalho (USC) ZHAireS and neutrino radio detection February 9th 2015 4 / 36

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SLIDE 5

ZHAireS and ZHAireS-Reflex Emission Mechanisms

Geomagnetic mechanism

Dominates emission in atmospheric showers Charged particles deflected by geomagnetic field B Emission from electrons and positrons add up

B v- v+ J- J+ J

F.D. Kahn and I. Lerche, Procs. Royal Society A 289 (1966) 206

Washington Carvalho (USC) ZHAireS and neutrino radio detection February 9th 2015 5 / 36

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SLIDE 6

ZHAireS and ZHAireS-Reflex The ZHAireS code

The ZHAireS code

ZHAireS (ZHS + Aires):

Simulation of radio emission in air showers and dense media (ice) Full shower simulation using Aires Radio emission calculation based on ZHS algorithms First microscopic simulation with refractive index n > 1 and varying n(h) Can easily simulate emission of neutrino induced showers (special primary)

AstropaPhys, 35, 325, 2012 and AstropaPhys, 35, 287, 2012

ZHS algorithms:

First principles (Maxwell) - No emission model presupposed. Geomagnetic, Charge Excess (Askaryan), etc... all included Frequency- and Time-domain calculations of vector potential A and electric field E

Zas, Halzen, Stanev, Phys.Rev.D V45, 362 (1992) and Phys.Rev.D81:123009,2010

Washington Carvalho (USC) ZHAireS and neutrino radio detection February 9th 2015 6 / 36

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SLIDE 7

ZHAireS and ZHAireS-Reflex The ZHAireS code

Extended ZHS algorithms: Time and Frequency domains

Time domain

  • A(t, ˆ

u) =

µe 4πRc

β⊥

Θ(t−tdet

1

)−Θ(t−tdet

2

) 1−n β·ˆ u

Frequency domain

  • E(ω, ˆ

u) = − µe

2πc

β⊥ eiω(t−tdet

1 )−eiω(t−tdet 2 )

1−n β·ˆ u û (const) R v

(const)

t1,E1,x1 t2,E2,x2 θ

  • 4
  • 3
  • 2
  • 1

1 2 3 4 5

  • 2
  • 1

1 2 3 4 5 6

A(x,t) (arb. units)

> C

(1

✁n ✂cos )(t2 ✁t1 ) ✄ec ☎sin ✆

4

✝(1 ✞n ☎cos ✆) < C
  • ✟
C
  • 4
  • 3
  • 2
  • 1

1 2 3 4 5

t✁nR/c (arb. units)

  • 6
  • 4
  • 2

2 4 6

E(x,t) (arb. units)

> C < C
  • ✟
C

E =

✁dA/dt

Santiago group, Phys.Rev.D81,123009 (2010)

Washington Carvalho (USC) ZHAireS and neutrino radio detection February 9th 2015 7 / 36

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SLIDE 8

ZHAireS and ZHAireS-Reflex Polarization and the Cherenkov ring

Polarization

Geomagnetic mechanism polarization ( G) Aproximatelly paralell to − V × B Independant of observer position Askaryan mechanism polarization ( A) Aproximatelly radial w.r.t. shower axis V Depends on observer position

B V A

(radial to V)

α θ (parallel to -V x B) G

Washington Carvalho (USC) ZHAireS and neutrino radio detection February 9th 2015 8 / 36

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SLIDE 9

ZHAireS and ZHAireS-Reflex Polarization and the Cherenkov ring

Superposition of emission mechanisms: Asymmetries

Vertical shower with horizontal B

N S W E

geo-magnetic Askaryan

Washington Carvalho (USC) ZHAireS and neutrino radio detection February 9th 2015 9 / 36

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SLIDE 10

ZHAireS and ZHAireS-Reflex Polarization and the Cherenkov ring

Superposition of emission mechanisms: Asymmetries

Vertical shower with horizontal B

N S W E

geo-magnetic Askaryan

Washington Carvalho (USC) ZHAireS and neutrino radio detection February 9th 2015 9 / 36

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SLIDE 11

ZHAireS and ZHAireS-Reflex Polarization and the Cherenkov ring

Superposition of emission mechanisms: Asymmetries

Vertical shower with horizontal B

North of core EW component: pure geomagnetic NS component: pure Askaryan

N S W E

geo-magnetic Askaryan

South of core EW component: pure geomagnetic NS component: pure Askaryan

Washington Carvalho (USC) ZHAireS and neutrino radio detection February 9th 2015 9 / 36

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SLIDE 12

ZHAireS and ZHAireS-Reflex Polarization and the Cherenkov ring

Superposition of emission mechanisms: Asymmetries

West of core Askaryan and geomagnetic have

  • pposite directions:

They subtract

Vertical shower with horizontal B

North of core EW component: pure geomagnetic NS component: pure Askaryan

N S W E

geo-magnetic Askaryan

South of core EW component: pure geomagnetic NS component: pure Askaryan

Washington Carvalho (USC) ZHAireS and neutrino radio detection February 9th 2015 9 / 36

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SLIDE 13

ZHAireS and ZHAireS-Reflex Polarization and the Cherenkov ring

Superposition of emission mechanisms: Asymmetries

West of core Askaryan and geomagnetic have

  • pposite directions:

They subtract

Vertical shower with horizontal B

North of core EW component: pure geomagnetic NS component: pure Askaryan

N S W E

geo-magnetic Askaryan

South of core EW component: pure geomagnetic NS component: pure Askaryan East of core Askaryan and geomagnetic are parallel: They add up

Washington Carvalho (USC) ZHAireS and neutrino radio detection February 9th 2015 9 / 36

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SLIDE 14

ZHAireS and ZHAireS-Reflex Polarization and the Cherenkov ring

Superposition of emission mechanisms: Asymmetries

West of core Askaryan and geomagnetic have

  • pposite directions:

They subtract

Vertical shower with horizontal B

North of core EW component: pure geomagnetic NS component: pure Askaryan

N S W E

geo-magnetic Askaryan

Net field

E=E(r,φ)

South of core EW component: pure geomagnetic NS component: pure Askaryan East of core Askaryan and geomagnetic are parallel: They add up

Washington Carvalho (USC) ZHAireS and neutrino radio detection February 9th 2015 9 / 36

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SLIDE 15

ZHAireS and ZHAireS-Reflex Polarization and the Cherenkov ring

Superposition of emission mechanisms: Asymmetries

N S W E

geo-magnetic Askaryan Net field

E=E(r,φ)

EW component NS component

  • Astropar. Phys., 35, (2012) 325

Washington Carvalho (USC) ZHAireS and neutrino radio detection February 9th 2015 10 / 36

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SLIDE 16

ZHAireS and ZHAireS-Reflex Polarization and the Cherenkov ring

Cherenkov Ring

Observers that see Xmax at θC

Define a ring-like region on the ground Maximum field amplitude Sizeable intensity well into the GHz range Ring is elliptical for non-vertical showers

Frequency (MHz) 200 400 600 800 1000 1200 1400 (V/m/MHz)

EW

E

  • 6

10

  • 5

10

  • 4

10

Cherenkov 100 m in 100 m out 200 m in 200 m out 400 m in 400 m out

In Out

~Xmax

Out

N S W E Shower Axis

Out Out

Coordinate (m)

  • 1500
  • 1000
  • 500

500 1000 1500 E (V/m/MHz) 0.00 0.02 0.04 0.06 0.08 0.10 0.12 0.14

  • 3

10 × 300 MHz EW Line NS Line

70◦ shower

  • J. Alvarez-Mu˜

niz, W. Carvalho Jr., A. Romero-Wolf, M. Tueros, E. Zas,

  • Phys. Rev. D 86 (2012) 123007

Washington Carvalho (USC) ZHAireS and neutrino radio detection February 9th 2015 11 / 36

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SLIDE 17

ZHAireS and ZHAireS-Reflex Some comparisons with data

ZHAireS simulations in good agreement with data

distance to shower axis [m] 100 200 300 400 500 600 700 V / m] µ | [ E | 500 1000 1500 2000 ZHAireS, SIBYLL 2.1 Measurement Proton Iron

ZHAireS simulation of AERA event Pierre Auger Collaboration, ICRC2013, id #899

Washington Carvalho (USC) ZHAireS and neutrino radio detection February 9th 2015 12 / 36

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SLIDE 18

ZHAireS and ZHAireS-Reflex Some comparisons with data

Very good agreement of the RLDF shape

LOFAR Xmax reconstruction using ZHAireS simulations (σXmax ∼ 20g/cm2)

Washington Carvalho (USC) ZHAireS and neutrino radio detection February 9th 2015 13 / 36

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SLIDE 19

ZHAireS and ZHAireS-Reflex The Two-component approach approximation

Two-component approach approximation

Significantly reduces computing time Based on superposition of Askaryan and geomagnetic components Field at any position extrapolated from few antenna simulations Very good agreement with full simulation for most geometries

W-E coordinate r (m)

  • 800
  • 600
  • 400
  • 200

200 400 600 800 | (V/m) E | 0.02 0.04 0.06 0.08 0.1 0.12 0.14 0.16 0.18 0.2

  • 3

10 ×

θ ° 70 ° 60 ° 45 ° 25 Full Sim

  • Astropar. Phys., 59 (2014) 29

Washington Carvalho (USC) ZHAireS and neutrino radio detection February 9th 2015 14 / 36

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SLIDE 20

ZHAireS and ZHAireS-Reflex ZHAireS-Reflex

ZHAireS-Reflex

Special ZHAireS code Reflection on ground (ice) and propagation to a high altitude detector Includes the Fresnel reflection coefficients

ice shower axis Ground antenna

ZHAireS

  • Astropar. Phys 66 (2015) 31-38

Washington Carvalho (USC) ZHAireS and neutrino radio detection February 9th 2015 15 / 36

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SLIDE 21

ZHAireS and ZHAireS-Reflex ZHAireS-Reflex

ZHAireS-Reflex

Special ZHAireS code Reflection on ground (ice) and propagation to a high altitude detector Includes the Fresnel reflection coefficients

ice shower axis

reflection points

(apply Fresnel coefficients)

ZHAireS-Reflex

  • Astropar. Phys 66 (2015) 31-38

Washington Carvalho (USC) ZHAireS and neutrino radio detection February 9th 2015 15 / 36

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SLIDE 22

ZHAireS and ZHAireS-Reflex ZHAireS-Reflex

Fresnel coefficients

] ° [ θ 20 40 60 80 Reflection Coefficient

  • 1
  • 0.5

0.5 1

r

||

r

No Fresnel coefficients ] ° [ ψ

  • 1.5
  • 1
  • 0.5

0.5 1 ]

  • 1

MHz

  • 2

[pW m

300MHz

Φ

  • 5

10

  • 4

10

  • 3

10

  • 2

10

  • 1

10 1 10

° =57 θ ° =64 θ ° =71 θ ° =78 θ ° =85 θ

With Fresnel coefficients ] ° [ ψ

  • 1
  • 0.5

0.5 1 ]

  • 1

MHz

  • 2

[pW m

300MHz

Φ

  • 6

10

  • 5

10

  • 4

10

  • 3

10

  • 2

10

  • 1

10 1

° =57 θ ° =64 θ ° =71 θ ° =78 θ ° =85 θ

  • Astropar. Phys 66 (2015) 31-38

Washington Carvalho (USC) ZHAireS and neutrino radio detection February 9th 2015 16 / 36

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SLIDE 23

ZHAireS and ZHAireS-Reflex ZHAireS-Reflex

Full reflection simulation vs. ground signal extrapolation

ice shower axis

reflection points

(apply Fresnel coefficients) R

Xmax

R’ Rr = R + R’

Extrapolation of ground "signal"

θ = 57◦

] ° [ ψ

  • 2
  • 1.5
  • 1
  • 0.5

0.5 1 1.5 2 ]

  • 1

MHz

  • 2

[pW m Φ

  • 6

10

  • 5

10

  • 4

10

  • 3

10

  • 2

10

  • 1

10

At Payload Extrapolation

  • Astropar. Phys 66 (2015) 31-38

Washington Carvalho (USC) ZHAireS and neutrino radio detection February 9th 2015 17 / 36

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SLIDE 24

ZHAireS and ZHAireS-Reflex ZHAireS-Reflex

Full reflection simulation vs. ground signal extrapolation

ice shower axis

reflection points

(apply Fresnel coefficients)

Full reflection calculation

θ = 57◦

] ° [ ψ

  • 2
  • 1.5
  • 1
  • 0.5

0.5 1 1.5 2 ]

  • 1

MHz

  • 2

[pW m Φ

  • 6

10

  • 5

10

  • 4

10

  • 3

10

  • 2

10

  • 1

10

At Payload Extrapolation

  • Astropar. Phys 66 (2015) 31-38

Washington Carvalho (USC) ZHAireS and neutrino radio detection February 9th 2015 17 / 36

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SLIDE 25

ZHAireS and ZHAireS-Reflex ZHAireS-Reflex

Summary

We now have a good undertanding of the radio emission of EAS ZHAireS can describe the details of this emission Good agreement with data A simple two-componnet approach can be used to drastically reduce computing time ZHAireS-Reflex performs full reflection simulations Fresnel coefficients of utmost importance Full reflection simulations differs considerably from ground signal extrapolation

Washington Carvalho (USC) ZHAireS and neutrino radio detection February 9th 2015 18 / 36

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SLIDE 26

Radio array sensitivity to Earth-Skimming ντ End to end simulation

Radio array sensitivity to Earth-Skimming ντ

Jaime Alvarez-Mu˜ niz1 Pablo Pieroni2

1Departamento de F´

ısica de Part´ ıculas & Instituto Galego de F´ ısica de Altas Enerx´ ıas Universidad de Santiago de Compostela, Espa˜ na.

2Departamento de F´

ısica - Facultad de Ciencias Exactas y Naturales Universidad de Buenos Aires, Argentina.

February 9th 2015

J.Alvarez-Mu˜ niz, P. Pieroni (USC-UBA) Radio array sensitivity to Earth-Skimming ντ February 9th 2015 19 / 36

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SLIDE 27

Radio array sensitivity to Earth-Skimming ντ End to end simulation

End to end simulation

Simulation stages

  • 3. ZHAireS
  • 4. Our code: Antenna response

Efficiency estimation

τ

  • 2. TAUOLA

Decay products

  • 1. Our code:

1

P(τ, ντ): Probability to obtain a τ with (Eτ, θ) given a ντ with (Eν, θ) using our code

2

τ decay products obtained with TAUOLA

3

Shower evolution and antenna signal calculation with ZHAireS

4

Antenna response and efficiency calculation using our code

J.Alvarez-Mu˜ niz, P. Pieroni (USC-UBA) Radio array sensitivity to Earth-Skimming ντ February 9th 2015 20 / 36

slide-28
SLIDE 28

Radio array sensitivity to Earth-Skimming ντ End to end simulation

Radio footprint

Cherenkov emision projected on the ground

Shower axis

Cherenkov cone

d 2 w

max

l h

max

l = 0

τ decay

θ

cher

d = 0 Width w of hyperbola: w2 =

  • tan2 θcher − tan2

θ − π 2 d sin θ − lmax 2 −tan

  • θ − π

2 hmax sin θ d sin θ − lmax

  • − h2

max

sin2 θ

J.Alvarez-Mu˜ niz, P. Pieroni (USC-UBA) Radio array sensitivity to Earth-Skimming ντ February 9th 2015 21 / 36

slide-29
SLIDE 29

Radio array sensitivity to Earth-Skimming ντ End to end simulation

Radio footprint

Energy of the tau that goes into shower ∼ 1 EeV

1

Very elongated and narrow footprints (hyperbola)

2

In agreement with prediction from simple model of Cherenkov cone emission

J.Alvarez-Mu˜ niz, P. Pieroni (USC-UBA) Radio array sensitivity to Earth-Skimming ντ February 9th 2015 22 / 36

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SLIDE 30

Radio array sensitivity to Earth-Skimming ντ Efficiency and Exposure

Efficiency calculation

J.Alvarez-Mu˜ niz, P. Pieroni (USC-UBA) Radio array sensitivity to Earth-Skimming ντ February 9th 2015 23 / 36

Shower energy: 1 EeV

Easting

  • 5000
  • 4000
  • 3000
  • 2000
  • 1000

1000 2000 3000 4000 5000 Northing

  • 5000
  • 4000
  • 3000
  • 2000
  • 1000

1000 2000 3000 4000 5000 Antennas 1000 core positions Easting

  • 20000
  • 10000

10000 20000 Northing

  • 20000
  • 10000

10000 20000 Antennas Triggered Antennas Footprint over Threshold

Example: Squared grid array. 900 m separation between antennas. Big enough to contain the whole radio footprint (hyperbola). 1000 random core positions in each (Eshower, θ, τdecay Height) bin. Antenna response 30 − 80 MHz/150 − 900 MHz. Trigger if n antennas above threshold (selected by user) Neutrino identification efficiency (conservatively) assumed to be 90%

Based on the apparent velocity of the signal and the width w of the footprint. Identification criteria not yet optimized

slide-31
SLIDE 31

Radio array sensitivity to Earth-Skimming ντ Efficiency and Exposure

Exposure calculation

Formula E(Eν) = 2πTA ∞ θmax

θcut

Eν Eτ ǫ(Xd, θ, Esh)e− l(Xd )

λ(Eτ )

λ(Eτ) dl(Xd) dXd P(Esh|Eτ) P(Eτ|Eν, θ)sin θ cos θdEshdEτdθdXd Ingredients Time and area Trigger and ν identification efficiency Probability of τ decay at vertical depth Xd in atmosphere. Probability of τ of energy Eτ producing shower of energy Esh Interaction of ντ inside Earth Solid angle

J.Alvarez-Mu˜ niz, P. Pieroni (USC-UBA) Radio array sensitivity to Earth-Skimming ντ February 9th 2015 24 / 36

slide-32
SLIDE 32

Radio array sensitivity to Earth-Skimming ντ Sensitivity of a radio array

Sensitivity of a radio array (3 yr)

Differential limit calculation Assume ν flux: Φν = k E −2

ν

⇒ Sensitivity =

2.4 E−2

ν

E(Eν)∆Eν with ∆Eν = half a decade in Eν

Radio array: 90,000 antennas, 900 × 900 m grid - Trigger threshold 50-350 µV/m

10

16

10

17

10

18

10

19

10

20

10

21

Eν[eV]

10

  • 9

10

  • 8

10

  • 7

10

  • 6

10

  • 5

E2 dN/ /dE [GeV2 cm−2 s−1 sr−1 ]

Single flavor

Fe, FRII & SFR (Kampert '12) p, Fermi-LAT (Ahlers '10) Waxman-Bachall '01 p & mixed (Kotera '10) IceCube 2013 Auger 2012 Anita-II 2010 Arianna 3yr ARA 3yr Radio Array 3yr (Este trabajo)

J.Alvarez-Mu˜ niz, P. Pieroni (USC-UBA) Radio array sensitivity to Earth-Skimming ντ February 9th 2015 25 / 36

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SLIDE 33

ZHAireS and neutrino radio detection The End

Questions?

Other applications of Radio...

Washington Carvalho (USC) ZHAireS and neutrino radio detection February 9th 2015 26 / 36

slide-34
SLIDE 34

Backup

Askaryan Mechanism

Dominates emission in dense media Electron and positron currents are opposite

e+ e- v v J- J+ J+ + J- = 0

  • v approx. paralell to shower axis

Emission is due to an excess of electrons in the shower

Shower front entrains electrons from medium

(Compton, Møller, Bhabba and positron anihilation)

G.A. Askaryan, Soviet JETP 21 (1965) 658

Washington Carvalho (USC) ZHAireS and neutrino radio detection February 9th 2015 27 / 36

slide-35
SLIDE 35

Backup

  • AAsk reflects the charge excess

ZHAireS: Ice νe cascade with E0 =10 EeV CC with 0.8E0 going into an e− (LPM!!!)

NIMA 662, S187-S190, (2010) - ARENA2010 | AAsk|

2e-09 4e-09 6e-09 8e-09 1e-08 1.2e-08

  • 80
  • 60
  • 40
  • 20

20 40 60 80

  • |A| (a.u.)

Time (ns) θC-10o θC+10o

Charge excess vs. atmospheric depth

2e+08 4e+08 6e+08 8e+08 1e+09 1000 2000 3000 4000 5000 6000 7000 8000 9000 Ne-Np Depth (g/cm-2) νe - 80% e- 20% jet

Washington Carvalho (USC) ZHAireS and neutrino radio detection February 9th 2015 28 / 36

slide-36
SLIDE 36

Backup

Cherenkov-like effects

Relativistic effects play crucial role in emission Stem from atmospheric refractive index n > 1 (n=1.000325 @ sea level) Shower front travels faster than emission Time reversal / multiple parts of EAS seen simultaneously Large “time compression” around part seen at θC = cos−1(1/n)

)

2

Atmospheric Depth (g/cm 100 200 300 400 500 600 700 800 900 1000 Time at antenna (ns) 2 4 6 8 10 12 14

n=1.0 n=1.0003 n=n(h) GH (a.u.) 1D shower: r=50m

  • Astropar. Phys., 35, (2012) 325

Washington Carvalho (USC) ZHAireS and neutrino radio detection February 9th 2015 29 / 36

slide-37
SLIDE 37

Backup

Two-component approach approximation

Significantly reduces computing time Superposition of Askaryan and geomagnetic components assuming their theoretical polarizations and elliptical symmetry Field at any position can be extrapolated from of a single line of antenna simulations Very good agreement with full simulation for most geometries

r r

Cher

Reference Line x y Antenna Cherenkov Ring RCher Reff z S h

  • w

e r A x i s

(East) (North)

Observer Line W-E coordinate r (m)

  • 800
  • 600
  • 400
  • 200

200 400 600 800 | (V/m) E | 0.02 0.04 0.06 0.08 0.1 0.12 0.14 0.16 0.18 0.2

  • 3

10 ×

θ ° 70 ° 60 ° 45 ° 25 Full Sim

  • Astropar. Phys., 59 (2014) 29

Washington Carvalho (USC) ZHAireS and neutrino radio detection February 9th 2015 30 / 36

slide-38
SLIDE 38

Backup

ANITA UHECR detection

Designed for detection of ν showers in antarctic ice detected 16 UHECR: 14 of them reflected on ice Compatible with Geomagnetic mechanism GHz emission due to time compression effects

Washington Carvalho (USC) ZHAireS and neutrino radio detection February 9th 2015 31 / 36

slide-39
SLIDE 39

Backup

USC: Long tradition in the radio technique

ZHS: First simulations of radio emission (Dense media-Askaryan)

1990: Zas (USC), Halzen (Univ. Winscosin) and Stanev (Univ. Delaware) Algorithm based on first principles Dense media, EM shower, Frequency domain Several later studies/developmnets

ZHAireS: ZHS + AIRES

2009: ZHS algorithm extended to the time domain and Fresnel approximation Full shower simulation (AIRES) Air Showers and Dense Media (TIERRAS) First microscopic simulation with refractive index n > 1 and varying n(h) 2013: Only simulation capable of simulating reflected events (ANITA, SWORD)

Washington Carvalho (USC) ZHAireS and neutrino radio detection February 9th 2015 32 / 36

slide-40
SLIDE 40

Backup Washington Carvalho (USC) ZHAireS and neutrino radio detection February 9th 2015 33 / 36

slide-41
SLIDE 41

Backup Washington Carvalho (USC) ZHAireS and neutrino radio detection February 9th 2015 34 / 36

slide-42
SLIDE 42

Backup Washington Carvalho (USC) ZHAireS and neutrino radio detection February 9th 2015 35 / 36

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SLIDE 43

Backup Washington Carvalho (USC) ZHAireS and neutrino radio detection February 9th 2015 36 / 36