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Atmospheric Effects in the Electromagnetic Component of the Secondary Cosmic Rays in the Pierre Auger Observatory J. Alvarez-Castillo 1 and J. F. Valdés-Galicia 1 , for the Pierre Auger Collaboration 2 IS@O, April 2011 1 Space Sciences, Geophysical Institute, UNAM, Mexico City, Mexico. 2 Pierre Auger Observatory, Malargüe, Mendoza, Argentina.

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Page 1: Atmospheric Effects in the Electromagnetic Component of the Secondary Cosmic Rays in the Pierre Auger Observatory J. Alvarez-Castillo 1 and J. F. Valdés-Galicia

Atmospheric Effects in the Electromagnetic Component of

the Secondary Cosmic Rays in the Pierre Auger Observatory

J. Alvarez-Castillo1 and J. F. Valdés-Galicia1, for the Pierre Auger Collaboration2

IS@O, April 2011

1 Space Sciences, Geophysical Institute, UNAM, Mexico City, Mexico.

2 Pierre Auger Observatory, Malargüe, Mendoza, Argentina.

Page 2: Atmospheric Effects in the Electromagnetic Component of the Secondary Cosmic Rays in the Pierre Auger Observatory J. Alvarez-Castillo 1 and J. F. Valdés-Galicia

History

Alexeenko et al. 1985, 2002

1985:−1% hard + 2% soft

2002: Different effects for hard and soft components.

Muraki et al., 2004The increase of the counting rate was only about 1%.

Aglietta et al., 1999Increase of 5% of the counting rate.

González & Valdés-Galicia, 2006Alvarez-Castillo & Valdés-Galicia, 2010Variations of ±0.5-1% of the counting rates on average for hard and soft components.

Alvarez-Castillo & Valdés-Galicia, this work

The increase of the counting rate was only about 1%.

Page 3: Atmospheric Effects in the Electromagnetic Component of the Secondary Cosmic Rays in the Pierre Auger Observatory J. Alvarez-Castillo 1 and J. F. Valdés-Galicia

The Pierre Auger Observatory

The Pierre Auger Observatory is located in the Southern Hemisphere, in the area of Malargüe city, Mendoza Province, Argentina.

The Auger Observatory consists of an array of 1,600 water Cherenkov detectors, on a 1.5 km in an hexagonal grid covering 3,000 km2. The surface detector network is complemented by fluorescence detectors and weather stations.

Page 4: Atmospheric Effects in the Electromagnetic Component of the Secondary Cosmic Rays in the Pierre Auger Observatory J. Alvarez-Castillo 1 and J. F. Valdés-Galicia

EF during Thunderstorms(TS) >1,000 V/m, EF in Quiet Days (QD) < 200 V/m.

Fluctuations are different: In QD the most important variation is the diurnal variation. In TS both disturbances are coupled.

Red= Electric Field (EF); Blue= CR (Cosmic Rays)

Thunderstorm

Quiet Day

Page 5: Atmospheric Effects in the Electromagnetic Component of the Secondary Cosmic Rays in the Pierre Auger Observatory J. Alvarez-Castillo 1 and J. F. Valdés-Galicia

Data Selection

1. CR close to the solar minimum (2007/11/27-2010/01/22).

2. Data with large variations in the geomagnetic field (kp > 20) and Forbush decreases were discarded.

3. Correction for pressure was made, other effects were not considered, as they are of minor importance.

4. TS were defined as measurements of |EF| > 800 V/m.

5. QD were selected considering measurements of |EF| < 200 V/m.

6. WD are considered with measurements of 200 < |EF| < 800 V/m.

7. Other atmospheric variables were considered (temperature, pressure and humidity).

8. Data resolution for this study is five minutes.

Page 6: Atmospheric Effects in the Electromagnetic Component of the Secondary Cosmic Rays in the Pierre Auger Observatory J. Alvarez-Castillo 1 and J. F. Valdés-Galicia

Methodology

All data during electric storms, quiet and windy days were filtered, removing the lowest frequencies.

An analysis of frequency-time (wavelet) was performed to the data, obtaining the periodicities of these.

Signals were compared in time and frequency.

One second SD scaler data were processed to eliminate anomalies due to jumps in the PMT baselines(Not considered in this presentation).

Page 7: Atmospheric Effects in the Electromagnetic Component of the Secondary Cosmic Rays in the Pierre Auger Observatory J. Alvarez-Castillo 1 and J. F. Valdés-Galicia

Filtered CR data (five minute resolution)

The Filtering of the CR data during a day with a thunderstorm (2007/12/25), is shown in the bottom panel, the two sigma level is exceeded from 13:45 to 19:10 UTC, when a TS occurred.

Trend

Original data

Filtered

2 σInterval of the effects of the Thunderstorm

Page 8: Atmospheric Effects in the Electromagnetic Component of the Secondary Cosmic Rays in the Pierre Auger Observatory J. Alvarez-Castillo 1 and J. F. Valdés-Galicia

Wavelet Spectrum

Note:

-Red noise is calculated dynamically considering each time series.

-Sigma normalization data.

Interval of the TS effects on the EM component

Time serie of normalized data

Spectrogram

highest power

lowest power

red noise

Page 9: Atmospheric Effects in the Electromagnetic Component of the Secondary Cosmic Rays in the Pierre Auger Observatory J. Alvarez-Castillo 1 and J. F. Valdés-Galicia

Wavelet analysis during thunderstorms (five minute resolution 25/12/2007)

Peaks in the Spectrum are at 5 hr, 2 hr and also around 30 min. Beyond 15 min. the signal is confused with the red noise level.

EF spectrum shows two peaks: one with a maximum around 30-45 min., another around 6 hours, below the red noise.

FLUCTUATIONS ARE MUCH STRONGER DURING TS

Page 10: Atmospheric Effects in the Electromagnetic Component of the Secondary Cosmic Rays in the Pierre Auger Observatory J. Alvarez-Castillo 1 and J. F. Valdés-Galicia

Temperature Humidity Pressure

Electric Field Cosmic Rays Wind Speed

Page 11: Atmospheric Effects in the Electromagnetic Component of the Secondary Cosmic Rays in the Pierre Auger Observatory J. Alvarez-Castillo 1 and J. F. Valdés-Galicia

Wavelet analysis in quiet days(five minute resolution 20/03/2008)

Two peaks are present: around 30 min and one hour. Other two peaks are close to the red noise level: 3.15 hours and 6 hours.

Periodicities in EF are: one around 20 minutes, another from 4 to 6 hours (maximum at 5 hours), and a small peak close to 3 hours.

FLUCTUATIONS ARE SPARSE,

HF IS UNCORRELATED

Page 12: Atmospheric Effects in the Electromagnetic Component of the Secondary Cosmic Rays in the Pierre Auger Observatory J. Alvarez-Castillo 1 and J. F. Valdés-Galicia

Temperature Humidity Pressure

Electric Field Cosmic Rays Wind Speed

Page 13: Atmospheric Effects in the Electromagnetic Component of the Secondary Cosmic Rays in the Pierre Auger Observatory J. Alvarez-Castillo 1 and J. F. Valdés-Galicia

Filtered data (2007/12/08)

Cosmic Rays

Electric Field

Wind Speed

Temperature

Relative Humidity

Pressure

Page 14: Atmospheric Effects in the Electromagnetic Component of the Secondary Cosmic Rays in the Pierre Auger Observatory J. Alvarez-Castillo 1 and J. F. Valdés-Galicia

Temperature Humidity Pressure

Electric Field Cosmic Rays Wind Speed

Page 15: Atmospheric Effects in the Electromagnetic Component of the Secondary Cosmic Rays in the Pierre Auger Observatory J. Alvarez-Castillo 1 and J. F. Valdés-Galicia

CR and EF summary

CR (hours) EF (hours)

< 0.5 < 0.5

0.5, 1 0.5-1

2 (not always), ~5 2 (not always), ~5

Quiet days:

HF VARIATIONS ARE UNCORRELATED.

Periodicities present:

Thunderstorms days:

WE SEE HARMONIC VARIATIONS

IN CR AND EF (TUNED)

Periodicities present:

CR (hours) EF (hours)

< 0.5 < 0.5

0.5, 1 0.5-1

2 (not always), ~4-5 2 (not always), ~4-5

We worked with 12 TS and 21 QD

Page 16: Atmospheric Effects in the Electromagnetic Component of the Secondary Cosmic Rays in the Pierre Auger Observatory J. Alvarez-Castillo 1 and J. F. Valdés-Galicia

Possible explanations for periodicities

The periodicities of 30min, in CR and EF could be related to electric field transitions, known to exist higher in the atmosphere (Israel, 1971)

The periodicities of half hour and less in EF and CR, with some intermittency, may be connected with microburst wind, that potentially carries large amounts of dust, whose composition in Malargüe is mostly iron (FIP 8 eV), that could be electrically charged (Rasmussen et al., 2009).

The 2 hour periodicity in CR and EF could be related to light and gentle wind, carrying charged particles and ions (Reiter, 1992). The CR variation of around 6 hours is due to the fourth harmonic diurnal variation of the EF.(Bhartendu, 1972).

Other low frequency variations in CR during TS may be due to rain. Rain droplets carry unstable particles that decay and contribute to changes in the flow of the CR; for this reason these variations are not present in the EF [Aglietta et al., 1999; Vernetto , 2001; Alexeenko et al., 2007].

Page 17: Atmospheric Effects in the Electromagnetic Component of the Secondary Cosmic Rays in the Pierre Auger Observatory J. Alvarez-Castillo 1 and J. F. Valdés-Galicia

The main contributions of this work are:

1. During thunderstorms electric field and cosmic rays variations are coupled.

2. The variations in the electric field are composed of two frequencies: a high frequency of a few minutes and a low frequency of a few hours.

The high frequency is intermittent and is due to the existence of high intensity EF (higher than ±4,000 V/m) during thunderstorms.

The low frequency may be connected to the wind flow that carries particles and ions that build the EF, it is present in QD. The atmospheric electric field is, to a significant extent, due to charged particles and ions in the air, that generally tend to have a net positive charge (Reiter, 1992).

3. The intermittent EF and CR fluctuations that are coincident may be connected with microburst wind, that potentially carries large amounts of dust and ions. (Rasmussen et al., 2009)

SUMMARY

Page 18: Atmospheric Effects in the Electromagnetic Component of the Secondary Cosmic Rays in the Pierre Auger Observatory J. Alvarez-Castillo 1 and J. F. Valdés-Galicia

Acknowledgments

The successful installation and commissioning of the Pierre Auger Observatory would not have been possible without the strong commitment and effort from the technical and administrative staff in Malargüe.

M. in P. Hernán Asorey and Dr. Xavier Bertou for technical support in the Auger observatory data in the Centro Atómico Bariloche (San Carlos de Bariloche, Río Negro, Argentina).

CONACYT (Consejo Nacional de Ciencia y Tecnología) for the scholarship awarded me for the completion of doctoral.

We are very grateful to the following agencies and organizations for financial support in the Pierre Auger Observatory:

Page 19: Atmospheric Effects in the Electromagnetic Component of the Secondary Cosmic Rays in the Pierre Auger Observatory J. Alvarez-Castillo 1 and J. F. Valdés-Galicia

Thank you very much for your kind attention!

Page 20: Atmospheric Effects in the Electromagnetic Component of the Secondary Cosmic Rays in the Pierre Auger Observatory J. Alvarez-Castillo 1 and J. F. Valdés-Galicia

Tank selection for one second data resolution

Page 21: Atmospheric Effects in the Electromagnetic Component of the Secondary Cosmic Rays in the Pierre Auger Observatory J. Alvarez-Castillo 1 and J. F. Valdés-Galicia

Wavelet analysis during thunderstorm(one second resolution)

Page 22: Atmospheric Effects in the Electromagnetic Component of the Secondary Cosmic Rays in the Pierre Auger Observatory J. Alvarez-Castillo 1 and J. F. Valdés-Galicia

SCR Global spectrum at high frequencies

Periodicities of 0-90 seconds

Periodicities of 0-20 seconds

Page 23: Atmospheric Effects in the Electromagnetic Component of the Secondary Cosmic Rays in the Pierre Auger Observatory J. Alvarez-Castillo 1 and J. F. Valdés-Galicia

Periodicities summary (secs)

Tank Below red noise level Close to red noise level Above red noise level

323 12, 20 3.5, 7.6 40

373 2.5, 7.5, 16, 24, 40 5

472 3.5, 30 8

479 2.5, 5, 10, 14 22, 48

577 2.5, 30, 64 6 12

701 3, 16, 26, 40 12

875 3.5, 6, 28 12 50

901 6, 10-14, 24, 50 3.5

974 2.8, 4, 12, 25, 50 7

1034 2.5-3.5, 4, 8-12, 19, 32

1053 2.5, 5, 6.5 16 32

1101 3.8, 7, 14, 19, 30

1198 3.8, 6, 12, 25 38

1365 3, 5, 12-14, 24-28, 32-44, 58-64 16

1605 2.5-4, 8, 13, 16, 28, 58

Page 24: Atmospheric Effects in the Electromagnetic Component of the Secondary Cosmic Rays in the Pierre Auger Observatory J. Alvarez-Castillo 1 and J. F. Valdés-Galicia

Electric field spectrum

The periodicities ranging from 4 to 64 seconds!!

Page 25: Atmospheric Effects in the Electromagnetic Component of the Secondary Cosmic Rays in the Pierre Auger Observatory J. Alvarez-Castillo 1 and J. F. Valdés-Galicia

Preliminary Results(one second resolution)

Temporal resolution data of a second are useful to see the effects of lightning on the electromagnetic component of cosmic rays.

Very large increases covering a range from 5-25 standard deviations, depending of the intensity of the discharge.

Much of the variation present in cosmic rays are caused by an electric effect, which can be: redistributions of charges, electric shock or resonant effects, in the range of 4-64 seconds.

Periodicities<4 sec in SCR, are possibly due to the Runaway Breakdown Process. The presence of a strong electric field in a thundercloud causes the acceleration of energetic electrons, which through collisions generate more fast electrons, which in turn will be also accelerated, causing a cascading effect that leads to a large flow of electrons producing the electric discharge (Gurevich et al, 1999).

Page 26: Atmospheric Effects in the Electromagnetic Component of the Secondary Cosmic Rays in the Pierre Auger Observatory J. Alvarez-Castillo 1 and J. F. Valdés-Galicia

A partir de un campo eléctrico de alta tensión, nace la A partir de un campo eléctrico de alta tensión, nace la formación de la descargaformación de la descarga

1

Departamento de Ciencias Espaciales

Page 27: Atmospheric Effects in the Electromagnetic Component of the Secondary Cosmic Rays in the Pierre Auger Observatory J. Alvarez-Castillo 1 and J. F. Valdés-Galicia

La constante de Ionizacion del aire

2

Departamento de Ciencias Espaciales

Page 28: Atmospheric Effects in the Electromagnetic Component of the Secondary Cosmic Rays in the Pierre Auger Observatory J. Alvarez-Castillo 1 and J. F. Valdés-Galicia

Genera una concentración de cargas puntual, donde aparecen los trazadores

3

Departamento de Ciencias Espaciales

Page 29: Atmospheric Effects in the Electromagnetic Component of the Secondary Cosmic Rays in the Pierre Auger Observatory J. Alvarez-Castillo 1 and J. F. Valdés-Galicia

y abren el camino ionizado de conexión, y la descarga eléctrica aparece

4

Departamento de Ciencias Espaciales

Page 30: Atmospheric Effects in the Electromagnetic Component of the Secondary Cosmic Rays in the Pierre Auger Observatory J. Alvarez-Castillo 1 and J. F. Valdés-Galicia

El aire queda saturado eléctricamente

5

Departamento de Ciencias Espaciales

Page 31: Atmospheric Effects in the Electromagnetic Component of the Secondary Cosmic Rays in the Pierre Auger Observatory J. Alvarez-Castillo 1 and J. F. Valdés-Galicia

Y el proceso se puede repetir mas rápidamente

6

Departamento de Ciencias Espaciales

Page 32: Atmospheric Effects in the Electromagnetic Component of the Secondary Cosmic Rays in the Pierre Auger Observatory J. Alvarez-Castillo 1 and J. F. Valdés-Galicia

Teniendo varias descargas, lo cual esta en función de la carga de la nube

7

Departamento de Ciencias Espaciales

Page 33: Atmospheric Effects in the Electromagnetic Component of the Secondary Cosmic Rays in the Pierre Auger Observatory J. Alvarez-Castillo 1 and J. F. Valdés-Galicia

Distribución Mundial de Descargas Eléctricas

Diariamente en el mundo se producen unas 44,000 tormentas y se generan mas de 8,000,000 de descargas

Departamento de Ciencias Espaciales

Page 34: Atmospheric Effects in the Electromagnetic Component of the Secondary Cosmic Rays in the Pierre Auger Observatory J. Alvarez-Castillo 1 and J. F. Valdés-Galicia

Curva de Carnegie según LIS

0

50000

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300000

0 4 8 12 16 20 24

Time(UT)

flash

es

SE Asia

Africa Americas

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100000

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300000

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Time(UT)

flash

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SE Asia

Africa Americas

SE Asia

Africa Americas

Departamento de Ciencias Espaciales

Page 35: Atmospheric Effects in the Electromagnetic Component of the Secondary Cosmic Rays in the Pierre Auger Observatory J. Alvarez-Castillo 1 and J. F. Valdés-Galicia

Tank You very much !!!Tank You very much !!!