The Gulmarg Neutron Monitor Ramesh Koul Astrophysical Sciences Division Bhabha Atomic Research Centre Mumbai 400 085.

Slides:

Advertisements

Similar presentations

Geiger-Muller detector and Ionization chamber

Advertisements

Investigation of daily variations of cosmic ray fluxes in the beginning of 24 th solar activity cycle Ashot Chilingarian, Bagrat Mailyan IHY-ISWI Regional.

Cosmic Ray Using for Monitoring and Forecasting Dangerous Solar Flare Events Lev I. Dorman (1, 2) 1. Israel Cosmic Ray & Space Weather Center and Emilio.

4/18 6:08 UT 4/17 6:09 UT Average polar cap flux North cap South cap… South cap South enter (need to modify search so we are here) South exit SAA Kress,

GLAST The GLAST Balloon Flight experiment was performed with the collaboration of NASA Goddard Space Flight Center, Stanford Linear Accelerator Center,

Radiation Detectors / Particle Detectors

Study of Galactic Cosmic Rays at high cutoff rigidity during solar cycle 23 Partha Chowdhury 1 and B.N. Dwivedi 2 1 Department of Physics, University.

Petukhov I.S., Petukhov S.I. Yu.G. Shafer Institute for Cosmophysical Research and Aeronomy SB RAS 21st European Cosmic Ray Symposium in Košice, Slovakia.

Paul Evenson, Waraporn Nuntiyakul,

EAS EXPERIMENT ON BOARD OF THE AIRBUS A380 J. N. Capdevielle, F. Cohen, PCC, College de France K. Jedrzejczak, B. Szabelska, J. Szabelski, T. Wibig The.

Cosmic rays in solar system By: Tiva Sharifi. Cosmic ray The earth atmosphere is bombarded with the energetic particles originating from the outer space.

Cosmic Rays Basic particle discovery. Cosmic Rays at Earth – Primaries (protons, nuclei) – Secondaries (pions) – Decay products (muons, photons, electrons)

Towards a European Infrastructure for Lunar Observatories Bremen, Wednesday 23 rd March 2005 A 3D cosmic ray detector on the Moon X. Moussas University.

High Altitude Research Laboratory Astrophysical Sciences Division Bhabha Atomic Research Centre Gulmarg Kashmir. M. A. Darzi.

Presented by Steve Kliewer Muon Lifetime Experiment: A Model.

Gravitational waves LIGO (Laser Interferometer Gravitational-Wave Observatory ) in Louisiana. A laser beam is.

Counting Cosmic Rays through the passage of matter By Edwin Antillon.

First Analysis of the Auger APF Light Source Eli Visbal (Carnegie Mellon University) Advisor: Stefan Westerhoff.

Neutron Monitor Detection Efficiency John Clem University of Delaware 2004 Annual CRONUS Collaboration Meeting.

From real-time to final data — Some thoughts on quality control Rolf Bütikofer, Erwin O. Flückiger University of Bern, Switzerland.

Sayfa 1 EP228 Particle Physics Department of Engineering Physics University of Gaziantep Dec 2014 Topic 5 Cosmic Connection Course web page

Status of Cosmic Rays Physics at the Knee Andrea Chiavassa Università and INFN Torino NOW 2006 Otranto 9-16 September 2006.

CR variation during the extreme events in November 2004 Belov (a), E. Eroshenko(a), G. Mariatos ©, H. Mavromichalaki ©, V.Yanke (a) (a) IZMIRAN), ,

Ground Level Enhancement of May 17, 2012 Observed at South Pole SH21A-2183 Takao Kuwabara 1,3 ; John Bieber 1 ; John Clem 1,3 ; Paul Evenson 1,3 ; Tom.

● The Roland Maze Project: School-Based Extensive Air Shower Network ● Hands on CERN events J. Szabelski The Andrzej Soltan Institute for Nuclear Studies,

Detection of cosmic rays in the SKALTA experiment Marek Bombara (P. J. Šafárik University Košice), Kysak, August 2011.

Keep the standard candle of electron observations burning Provide an intercalibration with PAMELA and AMS Search for the origin of the turn up in the low.

The PLANETOCOSMICS Geant4 application L. Desorgher Physikalisches Institut, University of Bern.

Why Neutrino ? High energy photons are absorbed beyond ~ 150Mpc   HE  LE  e - e + HE s are unique to probe HE processes in the vicinity of cosmic.

Cosmic-Ray Induced Neutrons: Recent Results from the Atmospheric Ionizing Radiation Measurements Aboard an ER-2 Airplane P. Goldhagen 1, J.M. Clem 2, J.W.

1 Observations of Charge Sign Dependence in Solar Modulation Kiruna 2011 LEE Low Energy Electrons P.I.C. June 30, 2010 John Clem and Paul Evenson.

By Dr. A. Mahrous Helwan University - EGYPT By Dr. A. Mahrous Helwan University - EGYPT.

Experiment Design SCIPP Teacher Workshop Mary Jo Nordyke August 2010.

High-Energy Ground Level Events Measured with Neutron Monitors and the Milagro Instrument James M. Ryan University of New Hampshire and the Milagro Collaboration.

Operation of the Space Environmental viewing and Analysis Network (Sevan) in 24-th Solar Activity Cycle A. Chilingarian A. Chilingarian Yerevan Physics.

NMDB - the European neutron monitor database Karl-Ludwig Klein, for the NMDB consortium.

Page 1 HEND science after 9 years in space. page 2 HEND/2001 Mars Odyssey HEND ( High Energy Neutron Detector ) was developed in Space Research Institute.

1 IDM2004 Edinburgh, 9 september 2004 Helenia Menghetti Bologna University and INFN Study of the muon-induced neutron background with the LVD detector.

Multi-TeV  -ray Astronomy with GRAPES-3 Pravata K Mohanty On behalf of the GRAPE-3 collaboration Tata Institute of Fundamental Research, Mumbai Workshop.

Aa GLAST Particle Astrophysics Collaboration Instrument Managed and Integrated at SLAC/Stanford University The Gamma-ray Large Area Space Telescope (GLAST)

Cosmic rays at sea level. There is in nearby interstellar space a flux of particles—mostly protons and atomic nuclei— travelling at almost the speed of.

Cosmic Rays Cosmic Rays at Sea-Level - Extensive Air Showers and the detection of cosmic rays.

Nov Beam Catcher in KOPIO (H. Mikata Kaon mini worksyop1 Beam Catcher in the KOPIO experiment Hideki Morii (Kyoto Univ.) for the KOPIO.

APRIM Chiang Mai July 28, 2011 Heliospheric Physics with IceTop Paul Evenson University of Delaware Department of Physics and Astronomy.

On the origin of the huge natural electron accelerators operated in the thunderclouds Ashot Chilingarian Artem Alikhanyan National Laboratory (Yerevan.

GLAST The GLAST Balloon Flight experiment was performed with the collaboration of NASA Goddard Space Flight Center, Stanford Linear Accelerator Center,

David Argento (some aspects of) cosmogenic nuclide production.

6/26/06David Gerstle1 Photon and Electron Cosmic Ray Flux Study David Gerstle LArTPC – Yale University Undergraduate.

Russian Aviation and Space Agency Institute for Space Research NASA 2001 Mars Odyssey page 1 Workshop HEND Radiation environment on Odyssey and.

Cosmic ray physics in ALICE Katherin Shtejer Díaz For the ALICE Collaboration LatinoAmerican Workshop on High Energy Physics: Particles and Strings, Havana,

Space Environmental Viewing and Analysis Network (SEVAN) Chilingarian 1, Ch.Angelov 2, K. Arakelyan 1, T.Arsov 2, Avakyan 1, S. Chilingaryan 1,4, K. A.Hovhanissyan.

Physical Description of IceTop 3 Nov IceTop Internal Review Madison, November 3-4, 2010 Physical Description of IceTop Paul Evenson, University.

February 7, Long Term Decline of South Pole Neutron Monitor Counting Rate – A Possible Magnetospheric Interpretation Paul Evenson, John Bieber,

AMIGA – A direct measurement of muons in Pierre Auger Observatory

31/03/2008Lancaster University1 Ultra-High-Energy Neutrino Astronomy From Simon Bevan University College London.

Extreme Event Symposium 2004 MAGNETOSPHERIC EFFECT in COSMIC RAYS DURING UNIQUE MAGNETIC STORM IN NOVEMBER Institute of Terrestrial Magnetism,

The Real-Time Neutron Monitor Database Christian T. Steigies (2), Karl-Ludwig Klein & Nicolas Fuller (1), on behalf of the NMDB team (1) Christian-Albrechts.

Modeling of secondary cosmic ray spectra for Solar Cycles 23

Cosmogenic Muon Background

Akhmatov Z.A1, Khokonov A.Kh1,2, Masaev M.B1, Romanenko V.S1.

Paul Evenson University of Delaware

Muons in IceCube PRELIMINARY

Project Structure Advanced Neutron Spectrometer on the International Space Station (ANS-ISS) Mark Christl NASA/MSFC Oct 23, 2015 Honolulu, HI 1 1.

Search for Cosmic Ray Anisotropy with the Alpha Magnetic Spectrometer on the International Space Station G. LA VACCA University of Milano-Bicocca.

R. Bucˇık , K. Kudela and S. N. Kuznetsov

Gamma-ray Albedo of the Moon Igor V. Moskalenko (Stanford) & Troy A

University of Delaware

Alexander Mishev & Ilya Usoskin

Application of neutron monitor data for space weather

NMDB - the European neutron monitor database

Presentation transcript:

The Gulmarg Neutron Monitor Ramesh Koul Astrophysical Sciences Division Bhabha Atomic Research Centre Mumbai

NM configurations # IGY 1957/58 eff. ~ 1.9% # NM eff. ~ 5.7% # He3 based # Gd doped liquid scintillator

Gulmarg Neutron Monitor (GNM) # Originally IGY type - 21xBF3 counters 40mm dia and 900mm length - ~ 0.3 sq.m area # Modified for dual use - Detection of Fusion neutrons from lightning D-D neutrons 2.5MeV - Low energy atmospheric neutron background Solar modulation effects

GNM main specifications # Location 36.04N, 74.24E, 2743m asl # High rigidity station (11.6 GV) # Modified IGY type instrument optimized for detection of 2.45 MeV fusion neutrons. # 21 BF3 counters 90cm long, 3.8cm dia # Surface area 30,000 sq.cm. # Top paraffin 8cm thick # Bottom paraffin 28cm thick # Count rate ~36000 per h with an atmospheric pressure coefficient of % per mbar

GNM schematic

Counter layout of the GNM

Paraffin thickness optimization

Pulse amplitude spectrum

Oct-Nov 2003 FD event

September 2005 FD event

Detector profile matching (GNM/ESOIR)

Solar wind velocity/GNM count rate (Sept 07-Aug 08)

World-wide Network of NM & SNT

Proposed multi-station Network of mini GRAPES arrays and Neutron Monitors # Mini arrays (8-16 detectors) at Guwahati, Darjeeling and Gulmarg for ultra-high energy showers. (GRAPES detectors) # NM at Ooty, Darjeeling and Gulmarg for CR and space-weather studies # expand the network in the next phase

Summary # The modified lead free Gulmarg Neutron Monitor responds well to solar modulation effects # Possibility of using such NM along with the GRAPES mini-arrays is being investigated.

Comparison between IGY and NM64 Neutron Monitors

The process begins in space with primary galactic cosmic rays entering the atmosphere after passing through the heliosphere (solar modulation) and geomagnetic field (rigidity cutoff). Most of these primaries are energetic enough to produce a nuclear or high energy interaction initiating a cascade of particles through the atmosphere. As the ensemble of cascades develop the particle density and the particle type distribution varies with atmospheric depth as shown in the Figure. The passage of each particle type through atmosphere is determined by different interaction channels. The dominate interaction depends on particle type, energy and material. The question remains, how does the Neutron Monitor respond to this particles ?? Above energies of 100MeV muons are the dominate species at sea-level, however when considering all energies neutrons dominate in numbers.