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Question Normalization of an isotropic flux in space  by valentina <valentina>,   03 Mar, 2009
Dear all,

I am simulating the interaction of a space telescope with the cosmic ray environment and, after a long discussion with my colleagues, I am a bit confused on the normalization process that translates the number of counts in my detector in unity of counts/cm^2 sec.

So I really appreciate if somebody could help me to clarify this topic!

I show here what is my normalization way.

I have an isotropic proton flux F:

F = prot /cm^2 sec sr

I run the protons from a sphere of radius R within an half cone angle q to increase the statistics. My spacecraft is placed within the emission angle, that is the spacecraft is placed within the sphere of radius r, with

r = tan(q) x R

The GPS macro is:

/gps/particle proton

/gps/pos/type Surface

/gps/pos/shape Sphere

/gps/pos/radius 50.0 m ---> R

/gps/pos/centre 0.0 0.0 0.0 mm

/gps/ang/type iso

/gps/ang/mintheta 0 rad

/gps/ang/maxtheta 0.01 rad ---> q

while the spectral shape is made via /gps/hist .

At the end of the run, I detect a number of counts C on the focal plane. If N is the number of emitted protons, we call the fraction of detected/emitted particles Eff:

Eff = C/N

In order to trasform the number C to a rate P in counts/sec, I apply this formula:

P = Eff x F x (4 x PI) x PI x r^2 counts/sec

Then I divide the count rate P by the detecting area Adet, and the final flux B is given by:

B = P/Adet counts/cm^2 sec

The same normalization can be achieved using the simulation time:

D = F x A_sphere x omega prot/sec

where:

- A_sphere = 4 x PI x R^2 (the source sphere)

- omega = 2 x PI x (1 - cos(q)) (solide angle of the emission cone)

Then we calculate the simulated time:

Time = N/D (sec)

The flux B on the focal plane is given by:

B = C/(Time x Adet) counts/cm^2 sec

My normalization way is based on what shown by Sullivan (1971).

Now my question is: is this the right way?

Thank you all for the help!

Best regards, Valentina

1 Feedback: Re: Normalization of an isotropic flux in space   (Giovanni Santin - 03 Mar, 2009)
1 Question: Re: Normalization of an isotropic flux in space   (valentina - 03 Mar, 2009)
(_ Note: Re: Normalization of an isotropic flux in space   (Juan - 04 Mar, 2009)
(_ Ok: Re: Normalization of an isotropic flux in space   (valentina - 04 Mar, 2009)
(_ None: Re: Normalization of an isotropic flux in space   (Juan - 04 Mar, 2009)
2 None: Re: Normalization of an isotropic flux in space   (Paul Nicholas Colin Gloster - 03 Mar, 2009)
Question gps sphere source   by Daniel Braun <Daniel Braun>,   09 Oct, 2008
Hallo,

I need to use a sphere as a particle source with the gps class.

and I want the particles to shoot just in the inside of the sphere maximally tangential to the sphere. They also should be distributed even on the surface of the sphere.

What is the best way to realize this?

Thanks for any help.

Regards Daniel

1 Feedback: Re: gps sphere source   (Giovanni Santin - 10 Oct, 2008)
2 Feedback: Re: gps sphere source   (Giovanni Santin - 10 Oct, 2008)
1 None: Re: gps sphere source   (Daniel Braun - 10 Oct, 2008)
1 Feedback: Re: gps sphere source   (Giovanni Santin - 16 Oct, 2008)
2 None: Re: gps sphere source   (Daniel Braun - 30 Oct, 2008)
Question dose depth curve  by Daniel Braun <Daniel Braun>,   12 Sep, 2008
Hello everybody,

I tried to get a Dose depth curve in an Aluminium Sphere and compared it with the one I get from www.Spenvis.oma.be.

But for a thin shield I get not enough Energy deposited and for a thick shield I get to much Energy deposited.

Does anybody know what the Problem is

My Physiks are

// // // $Id: ExN03PhysicsList.cc,v 1.21 2007/07/02 13:22:08 vnivanch Exp $ // GEANT4 tag $Name: geant4-09-01-patch-02 $ // //

//....oooOO0OOooo........oooOO0OOooo........oooOO0OOooo........oooOO0OOooo...... //....oooOO0OOooo........oooOO0OOooo........oooOO0OOooo........oooOO0OOooo......

#include "ExN03PhysicsList.hh"

#include "G4ProcessManager.hh"
#include "G4ParticleTypes.hh"

//....oooOO0OOooo........oooOO0OOooo........oooOO0OOooo........oooOO0OOooo......

ExN03PhysicsList::ExN03PhysicsList():  G4VUserPhysicsList()
{
  defaultCutValue = 1*mm;
  SetVerboseLevel(1);
}

//....oooOO0OOooo........oooOO0OOooo........oooOO0OOooo........oooOO0OOooo......

ExN03PhysicsList::~ExN03PhysicsList() {}

//....oooOO0OOooo........oooOO0OOooo........oooOO0OOooo........oooOO0OOooo......

void ExN03PhysicsList::ConstructParticle()
{
  // In this method, static member functions should be called
  // for all particles which you want to use.
  // This ensures that objects of these particle types will be
  // created in the program. 

  ConstructBosons();
  ConstructLeptons();
  ConstructMesons();
  ConstructBaryons();
}

//....oooOO0OOooo........oooOO0OOooo........oooOO0OOooo........oooOO0OOooo......

void ExN03PhysicsList::ConstructBosons()
{
  // pseudo-particles
  G4Geantino::GeantinoDefinition();
  G4ChargedGeantino::ChargedGeantinoDefinition();

  // gamma
  G4Gamma::GammaDefinition();

  // optical photon
  G4OpticalPhoton::OpticalPhotonDefinition();
}

//....oooOO0OOooo........oooOO0OOooo........oooOO0OOooo........oooOO0OOooo......

void ExN03PhysicsList::ConstructLeptons()
{
  // leptons
  G4Electron::ElectronDefinition();
  G4Positron::PositronDefinition();
  G4MuonPlus::MuonPlusDefinition();
  G4MuonMinus::MuonMinusDefinition();

  G4NeutrinoE::NeutrinoEDefinition();
  G4AntiNeutrinoE::AntiNeutrinoEDefinition();
  G4NeutrinoMu::NeutrinoMuDefinition();
  G4AntiNeutrinoMu::AntiNeutrinoMuDefinition();
}

//....oooOO0OOooo........oooOO0OOooo........oooOO0OOooo........oooOO0OOooo......

void ExN03PhysicsList::ConstructMesons()
{
 //  mesons
  G4PionPlus::PionPlusDefinition();
  G4PionMinus::PionMinusDefinition();
  G4PionZero::PionZeroDefinition();
  G4Eta::EtaDefinition();
  G4EtaPrime::EtaPrimeDefinition();
  G4KaonPlus::KaonPlusDefinition();
  G4KaonMinus::KaonMinusDefinition();
  G4KaonZero::KaonZeroDefinition();
  G4AntiKaonZero::AntiKaonZeroDefinition();
  G4KaonZeroLong::KaonZeroLongDefinition();
  G4KaonZeroShort::KaonZeroShortDefinition();
}

//....oooOO0OOooo........oooOO0OOooo........oooOO0OOooo........oooOO0OOooo......

void ExN03PhysicsList::ConstructBaryons()
{
  //  barions
  G4Proton::ProtonDefinition();
  G4AntiProton::AntiProtonDefinition();
  G4Neutron::NeutronDefinition();
  G4AntiNeutron::AntiNeutronDefinition();
}

//....oooOO0OOooo........oooOO0OOooo........oooOO0OOooo........oooOO0OOooo......

void ExN03PhysicsList::ConstructProcess()
{
  AddTransportation();
  ConstructEM();
  ConstructDecay();
}

//....oooOO0OOooo........oooOO0OOooo........oooOO0OOooo........oooOO0OOooo......

#include "G4ComptonScattering.hh"
#include "G4GammaConversion.hh"
#include "G4PhotoElectricEffect.hh"

#include "G4MultipleScattering.hh"

#include "G4eIonisation.hh"
#include "G4eBremsstrahlung.hh"
#include "G4eplusAnnihilation.hh"

#include "G4MuIonisation.hh"
#include "G4MuBremsstrahlung.hh"
#include "G4MuPairProduction.hh"

#include "G4hIonisation.hh"

#include "G4LowEnergyIonisation.hh" 
#include "G4LowEnergyBremsstrahlung.hh" 

//....oooOO0OOooo........oooOO0OOooo........oooOO0OOooo........oooOO0OOooo......

void ExN03PhysicsList::ConstructEM()
{
  theParticleIterator->reset();
  while( (*theParticleIterator)() ){
    G4ParticleDefinition* particle = theParticleIterator->value();
    G4ProcessManager* pmanager = particle->GetProcessManager();
    G4String particleName = particle->GetParticleName();

    if (particleName == "gamma") {
      // gamma         
      pmanager->AddDiscreteProcess(new G4PhotoElectricEffect);
      pmanager->AddDiscreteProcess(new G4ComptonScattering);
      pmanager->AddDiscreteProcess(new G4GammaConversion);
      //pmanager->AddProcess(new G4eBremsstrahlung,   -1, 3,3);

    } else if (particleName == "e-") {
      //electron
      pmanager->AddProcess(new G4MultipleScattering,-1, 1,1);
      pmanager->AddProcess(new G4eIonisation,       -1, 2,2);
      pmanager->AddProcess(new G4eBremsstrahlung,   -1, 3,3);      

    } else if (particleName == "e+") {
      //positron
      pmanager->AddProcess(new G4MultipleScattering,-1, 1,1);
      pmanager->AddProcess(new G4eIonisation,       -1, 2,2);
      pmanager->AddProcess(new G4eBremsstrahlung,   -1, 3,3);
      pmanager->AddProcess(new G4eplusAnnihilation,  0,-1,4);

    } else if( particleName == "mu+" || 
               particleName == "mu-"    ) {
      //muon  
      pmanager->AddProcess(new G4MultipleScattering,-1, 1,1);
      pmanager->AddProcess(new G4MuIonisation,      -1, 2,2);
      pmanager->AddProcess(new G4MuBremsstrahlung,  -1, 3,3);
      pmanager->AddProcess(new G4MuPairProduction,  -1, 4,4);       

    } else if ((!particle->IsShortLived()) &&
	       (particle->GetPDGCharge() != 0.0) && 
	       (particle->GetParticleName() != "chargedgeantino")) {
      //all others charged particles except geantino
      pmanager->AddProcess(new G4MultipleScattering,-1, 1,1);
      pmanager->AddProcess(new G4hIonisation,       -1, 2,2); 

    }
  }
}

//....oooOO0OOooo........oooOO0OOooo........oooOO0OOooo........oooOO0OOooo......

#include "G4Decay.hh"

void ExN03PhysicsList::ConstructDecay()
{
  // Add Decay Process
  G4Decay* theDecayProcess = new G4Decay();
  theParticleIterator->reset();
  while( (*theParticleIterator)() ){
    G4ParticleDefinition* particle = theParticleIterator->value();
    G4ProcessManager* pmanager = particle->GetProcessManager();
    if (theDecayProcess->IsApplicable(*particle)) { 
      pmanager ->AddProcess(theDecayProcess);
      // set ordering for PostStepDoIt and AtRestDoIt
      pmanager ->SetProcessOrdering(theDecayProcess, idxPostStep);
      pmanager ->SetProcessOrdering(theDecayProcess, idxAtRest);
    }
  }
}

//....oooOO0OOooo........oooOO0OOooo........oooOO0OOooo........oooOO0OOooo......

void ExN03PhysicsList::SetCuts()
{
  if (verboseLevel >0){
    G4cout << "ExN03PhysicsList::SetCuts:";
    G4cout << "CutLength : " << G4BestUnit(defaultCutValue,"Length") << G4endl;
  }

  // set cut values for gamma at first and for e- second and next for e+,
  // because some processes for e+/e- need cut values for gamma
  //

G4double lowlimit=250*eV;
  G4ProductionCutsTable::GetProductionCutsTable()
    ->SetEnergyRange(lowlimit, 100.*GeV);

  // default cuts for world volume
  G4double cutValue = 1*mm;
  SetCutValue(cutValue,"gamma");
  SetCutValue(cutValue,"e-");
  SetCutValue(cutValue,"e+");

  if (verboseLevel>0) DumpCutValuesTable();
}

//....oooOO0OOooo........oooOO0OOooo........oooOO0OOooo........oooOO0OOooo......

From my Detector Construction

I use aluminium as shield and Silicon as detector Material defined like this.

new G4Material("Aluminium", z=13., a=26.98*g/mole, density=2.70*g/cm3); new G4Material("Silicon" , z=14., a= 28.09*g/mole, density= 2.33*g/cm3);

I'm new with geant4 and don't have a clue where the mistake could be.

Thanks for any help

Kind regards

Daniel

1 None: Re: dose depth curve   (michel maire - 12 Sep, 2008)
(_ None: Re: dose depth curve   (Daniel Braun - 12 Sep, 2008)
(_ None: Re: dose depth curve   (Hugh Evans - 15 Sep, 2008)
(_ None: Re: dose depth curve   (Daniel Braun - 16 Sep, 2008)
(_ None: Re: dose depth curve   (Hugh Evans - 17 Sep, 2008)
(_ None: Re: dose depth curve   (Daniel Braun - 22 Sep, 2008)
None SPE Primary Particles   by Steven Avery <Steven Avery>,   21 Apr, 2008

I'm using the radioprotection example but I would like to only use solar particle events (SPE) as my primary particle. The example only has ascii files for galactic cosmic rays (GCR) data. How do I set the example to only generate SPE events?

1 Feedback: Re: SPE Primary Particles   (Giovanni Santin - 21 Apr, 2008)
Question Grazing angle proton scattering  by valentina <valentina>,   13 Feb, 2008

Hi, I have a question about the simulation of grazing angle proton scattering.

In the article:

"Low Angle Scattering of Protons on the XMM-Newton Optics and Effects on the On-Board CCD detectors"

Nartallo et al. 2001

Nartallo uses the multiple scattering to simulate the interaction of protons with a mirror reflecting surface layer (in this case XMM-Newton optics).

As a conseguence of:

"Grazing Angle Proton Scattering: effects on Chandra and XMM-Newton X-ray telescopes"

Dichter and Woolf, 2003

, where the authors show that the multiple scattering under predicts the expected proton flux at the focal plane,

Nartallo in the article:

"Update on the use of Geant4 for the simulation of low energy protons scattering off X-ray mirrors at grazing incidence angles"

implements a new physics process, G4FirsovScattering, in the G4 Monte Carlo code, to treat the scattering of low energy protons at grazing incidence angles.

Now the question is: someone knows where is G4FirsovScattering? I can't find it in G4 library!

Thanks!

Valentina

None Generating a Pulse height spectra through GEANT  Keywords: Getting a Pulse height spectra from GEANT
by rajani <rajani>,   02 Feb, 2007

Hi All!!

In a normal space experiment, the particles ( suppose photons here) interact with the detector, giving rise to the absorption or transmission of the particle. In GEANT, we can trace the physics processes it undergoes, the energy it carries after that & the step at which it does that. In a Lab- experiment, what we get out is a Pulse Height Spectra that tells the variation of no of counts with the voltage, My concern is, Can GEANT in any way tell me about the Pulse height spectra? If yes, Can you tell me how & the reference? Thanking You

Rajani

1 None: Re: Generating a Pulse height spectra through GEANT   (Maria Grazia Pia - 02 Feb, 2007)
Question Sunyaev-Zeldowich effect and GEANT4  Keywords: Cosmology, Astroparticle Physics
by Forough <Forough>,   22 Nov, 2006
   Hi,
   We are going to use GEANT4 in scattering of electrons
   from ionized atoms, so-called Sunyaev-Zeldowich effect
   in cosmology and astroparticle physics.
   Up to the best of our knowledge, this topic has not been
   worked until now. We are pleased to receive your comments
   about the application of GEANT4 in Sunyaev-Zeldowoch effect.
   Could you please help us? 
   Thanks if you reply.
   Sincerely,
   Forough Nasseri
Question hemisphere generation using General Particle Source Module  Keywords: hemisphere in gps
by Manju Sudhakar <manjus@isac.gov.in>,   28 Aug, 2006

Hi,

I would like to know how to generate a hemisphere using General Particle Source Module. It is easy to do so in the G4UserPrimaryGeneratorAction.cc, but I want to use gps because my energy is in the form of a user defined histogram. I checked the queries posted in this forum regarding generation of a hemisphere using gps, and I found out that "biasing" should be used and the extended example "exgps" has a macro "test32.g4mac, which gives the methodology to do so. But, I donot know how the biasing works and the gps manual doesnot give any details. Could someone please help me out in this.. It is really important, as I want to model the space-craft background due to photons generated on the inner surface of a hemisphere that is placed behind the space-craft, ie, the photons are incident from the hemisphere inner surface and impinging on the back of the detector.

Please could someone tell me how to go about this ??

Thanks, Manju Sudhakar.

None Physics Process to include to take care of x-ray polarization  by Manju Sudhakar <manjus@isac.gov.in>,   30 May, 2006

Hi,

I am working on a first step x-ray polarimeter design.I want to measure the polarization of low energy x-rays after scattering from a target. So, inorder to do that, I need to include, in the physics list a process that takes care of polarization. There is a physics process "G4LowEnergyPolarizedComptonScattering", but it is not used in any of the examples ..

And another thing is that in the http://geant4.esa.int/events/g4suw03/ site, there are a number of presentations that mention polarized photoelectric, Rayleigh scattering, pair production etc. And in the photoelectric presentation , there is a page where they show the actual track of the photon, and it is mentioned "G4LowEnergyPolarizedPhotoelectric".

I am using GEANT version 4.7.0.p01.
In the directory /geant4/geant4.7.0.p01/source/processes/electromagnetic/lowenergy/include, 
the only low energy polarization physics process is G4LowEnergyPolarizedComptonScattering
is there. Also, there is no PolarizationManager. In the paper by Ralph Dollan, Karim Laihem 
and Andreas Schalicke "Monte Carlo based studies of a polarized positron 
source for International Linear Collider (ILC)" (arXiv:physics/0512192 v1), they talk about 
polarization framework in GEANT4 .. They talk about "proposed implementation of polarized processes" 
 ... so are these yet to be implemented ?? In the latest version of GEANT, 
are these implemented ??

So, in the version of GEANT that I am using, 4.7.0.p01, the only physics process that is available is "G4LowEnergyPolarizedComptonScattering".

Could you please give me more information about the proposed implementation of polarization ? Is it already implemented ?

Thanks in advance, Manju Sudhakar.

1 None: Re: Physics Process to include to take care of x-ray polarization   (Maria Grazia Pia - 02 Jun, 2006)
None Geant4 applications at IEEE NSS 2006  by Maria Grazia Pia <Maria Grazia Pia>,   29 May, 2006

Geant4 users in space applications may be interested to submit an abstract on their ongoing projects to the IEEE Nuclear Science Symposium (http://www.nss-mic.org/2006). IEEE NSS is a major conference in experimental technologies, including a Software & Computing session. This year it will take place in San Diego, the week before the SPENVIS-Geant4 Space User Workshop also hosted in California in 2006.

The official deadline for abstract submission is over, but direct submission to the conveners is still accepted.

If you are interested, please send your abstract to the Software and Computing convener (Maria.Grazia.Pia@cern.ch, with cc to nss2006@ornl.gov).

Looking forward to many exciting Geant4 results,

Maria Grazia Pia

NSS Software & Computing co-Convener

None regarding polarization in gps  by Manju Sudhakar <manjus@isac.gov.in>,   25 May, 2006

Hi,

This is the first time I will be simulating polarization and I'll be doing it using gps.

The command /gps/polarizarion Px Py Pz where Px, Py and Pz are the doubles that sets the polarization of the source .. Are these the Stokes parameters ?? The parameters for linear polarization, circular polarization and elliptical polarization ..So if my source photons are linearly polarized only, then the values for Px, Py and Pz would be 1,0,0 .. Is my understanding correct or is this something else ...??? These are not vectors ..but doubles .. Could you help me out ??

Regards and thanks, Manju Sudhakar

 

Question How to define the flux of particles?  Keywords: flux
by Lee Xuesheng <chaosl@pku.edu.cn>,   06 Mar, 2006

When using the geant4 in application for Space Radiation,how can I define the flux of particles(e- or gamma)? thanks

1 None: Re: How to define the flux of particles?   (Hugh Evans - 07 Mar, 2006)
1 None: Re: How to define the flux of particles?   (Andres - 25 Mar, 2006)
3 None: Re: How to define the flux of particles?   (Andres - 25 Mar, 2006)
1 None: Re: How to define the flux of particles?   (Hugh Evans - 27 Mar, 2006)
...
2 None: Re: How to define the flux of particles?   (Lee Xuesheng - 05 Oct, 2006)
...
None Untitled  by Andres <Andres.Russu@uv.es>,   06 Feb, 2006

I have two questions about spacecraft geant simulation.

1.- The number of particles. I am using gps and sphere source with spenvis histogram but I am not sure how many particles per second I have to simulate.

2.- Long term radiation. I would like to simulate long term secondary particles coming from the desactivation of the ISS materials. Do you have any idea about how to do this?

Thanks

1 None: Re: Untitled   (Hugh Evans - 06 Feb, 2006)
(_ None: Re: Untitled   (Andres.Russu@uv.es - 22 Feb, 2006)
None Spacecraft activation from bkg environment  by <Andres.Russu@uv.es>,   31 Jan, 2006

Dear friends,

I am simulating a gamma instrument for the ISS. I would like to simulate how the spacecraft is getting radioactive in a long term simulation. I mean I want to take into account the particles coming form the decays of the materials around the detector plane.

Thanks in advance, Andres

Question doubt concerning the radioactive decay  Keywords: energy deposit by radioactive decay as a function of time
by Manju Sudhakar <manjus@isac.gov.in>,   02 Jan, 2006
Hi, 

   I would like to simulate the spallation reactions that occur CsI detectors 
due to cosmic ray protons.First I want to do an experiment on the energy deposited 
in CsI due to irradiation by a beam of monoenergetic protons, as a function of time.
I want to get the energy deposit spectrum in CsI after irradiation, as a function of time.

    I have looked at the examples/extended/radioactivity/exrdm, where the concept of 
theStep->GetPreStepPoint()->GetGlobalTime() is used.

Please, could someone help me in understanding this concept and how it is used in 
radioactive decay ????
How can I use this to get the energy deposit as a function of time since irradiation ???
Could someone please answer my query ...

With thanks, 
Manju Sudhakar.
Question doubts concerning grdm  Keywords: doubts about grdm commands
by Manju Sudhakar <manjus@isac.gov.in>,   29 Dec, 2005
Hi, 
  I would like to simulate the decay of induced radio-isotopes when protons 
are incident on a space-borne gamma-ray detector, cosmic-ray protons.I want 
to model the detector background.To simulate radioactive decay, we need to 
use grdm.There are some aspects about it I don't understand.

1) the command /grdm/sourceTimeProfile <filename>
    
    as given in the manual, it is for defining the "source time profile"
I donot understand ... what does this mean ?? Why is it used ?? Is it 
mandatory ?? In the extended example "radioactivity/exrdm" in geant 4.7.0, 
in one of the macros "proton-b.mac" /grdm/sourceTimeProfile beam.data is a 
command.When I opened beam.data, the file looked like this 
0  1e6
60  0

Donot understand head or tail of this ... please help me get clarified on 
this point.


2) the command /grdm/decayBiasProfile <filename>

       What about this command ?In the extended example "radioactivity/exrdm" 
in geant 4.7.0, in the macro "proton-b.mac", there is a command 
/grdm/decayBiasProfile measures.data.And, when I opened it
1000     1
1100     0
3000     1
3100     0
1e5      1
1.1e5    0

    No clue to what this file means.

Could someone please explain all this to me clearly and in detail ?

With lots and lots of advance thanks 
Manju Sudhakar.
None Re: Doubt regarding General Particle Source Module  by Hugh Evans <Hugh Evans>,   30 Aug, 2005
Hello Manju,

The energy units in the GPS histogram that you're building are in MeV. The
absolute values of the differential "flux" are not important as they are all
normalised to a probability distribution [0..1], therefore the relative
difference between bins in the histogram are of the greatest importance, not
the absolute value.

While cosmic ray fluxes aren't yet available, the trapped proton, trapped
electron and solar proton flux/fluence spectra from SPENVIS
(http://www.spenvis.oma.be/spenvis/) can be converted to GPS macros via its
Mulassis application.  By playing with this, you can easily determine how the
environmental spectra are converted to the GPS macro commands.

Alternatively, I can also send you an Excel spreadsheet within which the
CREME-86 spectra are implemented and the GPS macros are formed.

Regards,
Hugh

-----
H. Evans
ESA/ESTEC/TEC-EES
Postbus 299
2200 AG Noordwijk
The Netherlands

Phone:+31 (0)71 565-5109
Fax:     +31 (0)71 565-4999



|---------+--------------------------->
|         |           Manju Sudhakar  |
|         |           <manjus@isac.ern|
|         |           et.in>          |
|         |                           |
|         |           30/08/2005 09:25|
|         |                           |
|---------+--------------------------->
  >--------------------------------------------------------------------------------------------------------------------------|
  |                                                                                                                          |
  |        To:      space_app-g4hn@slac.stanford.edu                                                                         |
  |        cc:                                                                                                               |
  |        Subject: Doubt regarding General Particle Source Module                                                           |
  >--------------------------------------------------------------------------------------------------------------------------|




*** Discussion title: Space Applications
Email replies to space_app-g4hn@slac.stanford.edu must include:
  In-Reply-To: <"/space_app/3"@geant4-hn.slac.stanford.edu>
  Subject: ...change this to be about your reply.

Dear GEANT users ,

I have a doubt regarding one of the commands in General Particle Source
Module.

I have constructed a detector system mounted on a space platform, and I
wish to irradiate it with cosmic-ray protons, at 1AU.I have the spectrum
of the protons with me and I have to enter the energy and flux as a
user-defined arbitrary point-wise function of the form, /gps/ene/type
Arb /gps/hist/type arb /gps/hist/point ...(energy) ... (flux) .... ....
.... .... /gps/hist/inter Lin /run/beamOn 100000

        This is fine, but my doubts are as follows ,
1) What is the default value of the energy points ? Is it MeV ?
2) What is the default value of the differential flux to be entered as in the

   second column ?

Could you please answer my doubts. Regards, Manju Sudhakar.





1 None: Re: Doubt regarding General Particle Source Module   (Andres - 28 Sep, 2005)
Question Doubt regarding General Particle Source Module  Keywords: units of differential spectrum in gps.
by Manju Sudhakar <manjus@isac.ernet.in>,   30 Aug, 2005

Dear GEANT users ,

I have a doubt regarding one of the commands in General Particle Source Module.

I have constructed a detector system mounted on a space platform, and I wish to irradiate it with cosmic-ray protons, at 1AU.I have the spectrum of the protons with me and I have to enter the energy and flux as a user-defined arbitrary point-wise function of the form, /gps/ene/type Arb /gps/hist/type arb /gps/hist/point ...(energy) ... (flux) .... .... .... .... /gps/hist/inter Lin /run/beamOn 100000

        This is fine, but my doubts are as follows ,
1) What is the default value of the energy points ? Is it MeV ?
2) What is the default value of the differential flux to be entered as in the 
   second column ? 

Could you please answer my doubts. Regards, Manju Sudhakar.

None Geant4 Space Users Workshop  by Makoto Asai <Makoto Asai>,   02 Jun, 2005
Dear colleague,

On 3-7 October 2005, a combined workshop for the SPENVIS and 
GEANT4 Space applications communities will be held in the 
historic university town of Leuven, Belgium. The workshop venue 
is the Faculty Club of the Catholic University, situated in the 
beautifully restored Grand Beguinage, a UNESCO World Heritage 
Site.

The SPENVIS workshop will take place on 3-4 Oct, the Geant4 
workshop will follow on 6-7 Oct, with a joint session in the 
morning of 5 Oct.

The SPENVIS workshop is the second in a series that started at 
ESTEC in 2002. The emphasis during the SPENVIS workshop will 
be on user experience and requirements for future developments. 
We aim for an informal workshop with a limited number of 
presentations (and a poster session) which can serve as starting 
points for round table discussions addressing specific
developments and applications. The programme is deliberately 
kept open to allow users to actively participate in the 
organisation. If you have inputs or suggestions for the workshop 
programme, please send a note to D.Heynderickx@oma.be .

Several GEANT4 based radiation effects packages are now available 
or under development, which are or will be implemented in the 
SPENVIS user interface. In view of these developments, we opted 
for a combined workshop where users and developers of both 
communities can meet and interact.

The GEANT4 Space Users' workshop follows the events organised 
at ESTEC in 2003 and Vanderbilt University in 2004. The focus 
will be on new results for component, sensor, and shielding 
analyses, as well as on developments for Exploration and Science 
missions. Users are invited to highlight new requirements based 
on their applications.

Registration is now open at:
 http://www.spenvis.oma.be/spenvis/workshop/workshop.html 
Workshop participants are invited to submit abstracts before 
1st September, via e-mail attachment in pdf format to 
D.Heynderickx@oma.be . Please indicate for which part of the 
workshop you are submitting, and your preference for oral or 
poster presentation (subject to the final decision of the 
scientific committee). Abstracts and a more detailed programme
will be put on-line when available.

More information on SPENVIS and GEANT4 space applications can 
be found at
 http://www.spenvis.oma.be/ 
and
 http://geant4.esa.int/ 
respectively.


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