Solar Event Simulations using the HAWC Scaler System

@inproceedings{EnquezRivera2015SolarES,
  title={Solar Event Simulations using the HAWC Scaler System},
  author={O. Enŕıquez-Rivera and Alejandro Lara and R. A. Caballero-Lopez},
  year={2015}
}
The High Altitude Water Cherenkov (HAWC) Observatory is an air shower array located near the volcano Sierra Negra in Mexico. The observatory has a scaler system sensitive to low energy cosmic rays (the geomagnetic cutoff for the site is 8 GV) suitable for conducting studies of solar or heliospheric transients such as Ground Level Enhancements (GLEs) and Forbush decreases. In this work we present the simulation of the HAWC response to these phenomena. We computed HAWC effective areas for… 
5 Citations

Figures and Tables from this paper

HAWC as a Ground-Based Space-Weather Observatory

The High Altitude Water Cherenkov (HAWC) gamma-ray observatory is located close to the equator (latitude $18^{\circ }$ N), at an altitude of 4100 m above sea level. HAWC has 295 water Cherenkov

Highlights from the High Altitude Water Cherenkov Observatory

The High Altitude Water Cherenkov (HAWC) Gamma-Ray Observatory was completed this year at a 4100-meter site on the flank of the Sierra Negra volcano in Mexico. HAWC is a water Cherenkov ground array

The High Altitude Water Cherenkov (HAWC) Observatory

Abstract HAWC is a continuously operated, wide field of view detector comprised of three hundred 188,000 liter water Cherenkov detectors, each instrumented with four photomultipliers providing charge

New Method to Calculate the Time Variation of the Force Field Parameter

Galactic cosmic rays (CRs) entering the heliosphere are affected by interplanetary magnetic fields and solar wind disturbances resulting in the modulation of the CR total flux observed in the inner

References

SHOWING 1-10 OF 13 REFERENCES

Observation of the March 2012 Forbush decrease with the engineering array of the High Altitude Water Cherenkov Observatory

Neutron monitors have reported the observation of a Forbush decrease on March 7, 2012. VAMOS, an engineering array built for the HAWC (High Altitude Water Cherenkov) Observatory, was operational at

The cosmic ray ground level enhancement of 6 November 1997.

Observation of GeV Solar Energetic Particles from the 1997 November 6 Event Using Milagrito

Milagrito was an extensive air-shower observatory that served as a prototype for the larger Milagro instrument. Milagrito operated from 1997 February to 1998 May. Although it was designed as a very

Features of relativistic solar proton spectra derived from ground level enhancement events (GLE) modeling

With the developed by the authors of a ground level enhancements events (GLE) modeling technique, the modeling study of 35 large GLEs for the period 1956 - 2006 has been carried out. The basic

Solar modulation of galactic cosmic rays, 2

The equations governing cosmic-ray modulation allowing for convection, diffusion, and energy changes are approximated with simpler, more manageable equations that describe the particle behavior in a

CORSIKA: A Monte Carlo code to simulate extensive air showers

CORSIKA: A Monte Carlo Code to Simulate Extensive Air Showers CORSIKA is a program for detailed simulation of extensive air showers initiated by high energy cosmic ray particles. Protons, light

THE COSMIC-RAY GROUND-LEVEL ENHANCEMENT OF 1989 SEPTEMBER 29

The ground-level enhancement (GLE) of 1989 September 29 is one of the largest of 71 solar energetic particle events observed by neutron monitors on Earth. It was smaller than the record-breaking GLE

Cosmic‐ray yield and response functions in the atmosphere

[1] Since the middle 1950s, neutron monitors have provided a continuous record of the intensity of secondary atmospheric particles produced by the primary cosmic radiation above the atmosphere. The

Solar modulation of galactic cosmic rays.