ESA Space Environment & Effects Analysis Section

1CHEP20009 February 2000

ESA Space Environment & Effects Analysis Section

and

9 February 2000 CHEP2000 2


and

Petteri NieminenESA/ESTEC

XMM analysis: E. Daly1, H. Evans1, S. Giani2, F. Lei3, R. Nartallo1,

J. Sørensen1, P.R. Truscott3

Space-specific C. Ferguson4, R. Gurriaran4, F. Lei3, modules: P.R. Truscott3

Low-E extensions: J. Apostolakis2, S. Chauvie5, S. Giani2, V. Ivantchenko6, V. Lefébure1,2, M. Maire7, M.G. Pia2,8, L. Urban2,9

1) ESA/ESTEC (NL) 4) Univ. Southampton (UK) 7) LAPP (F)2) CERN (CH) 5) Univ. Torino (I) 8) INFN Genova (I)3) DERA (UK) 6) Budker Inst. For Nuclear Physics (RUS) 9) KFKI (HUN)

CHEP2000 3

Solar flare electrons,protons, and heavy ions

Jovianelectrons

Solar flare neutronsand -rays

SolarX-rays

Galactic and extra-galacticcosmic rays

Induced emission

(Neutrinos)

Trapped particles

Anomalouscosmic rays



Simulation “agenda”:

Spacecraft and instrument shielding properties Detector background effects in astrophysical observatories (including

from radioactive decay) Single Event Effects and total dose in sensitive components 3-D spacecraft design and radiation response verification Mineralogical surveys of asteroids and moons by induced X-ray line

emission Astronaut hazards: radiation effects at cellular and DNA level



Sector Shielding Analysis Tool

Low-energy e-m extensions

CAD tool front-end

Delayed radioactivity

General purpose source particle module

INTEGRAL and other science missions

Instrument design purposes Dose calculations

Particle source and spectrum

Geological surveys of asteroids



X-Ray Surveys of Asteroids and Moons

Induced X-ray line emission:indicator of target composition(~100 m surface layer)

Cosmic rays,jovian electrons

Geant3.21

ITS3.0, EGS4

Geant4

Solar X-rays, e, p

Courtesy SOHO EIT

C, N, O line emissions included



Low-E e-m models (electrons and photons)



Low-E e-m models (protons and ions)

Applications in the medical field, astrophysics, fundamental physics,...


X-ray Multi-Mirror mission(XMM)

Launch December 1999 Perigee 7000 km, apogee 114000 km Flight through the radiation belts Chandra X-ray observatory, with

similar orbit, experienced unexpected degradation of CCDs

Possible effects on XMM?Baffles

X-ray detectors(CCDs)

Mirrors

Telescope tube



Low-E (~100 keV to few MeV), low-angle (~0°-5°) proton scattering:Obscure problem; not much analysed

CCD displacement damage: front vs. back-illuminated.

30 m 2 m30 m2 m

30 m Si ~1.5 MeV p+

Active layerPassive layer

Basic geometry and co-ordinate system of theTRIM/Geant4 simulations.

θ

βα

X

YZ

“Electron deflector”



EPIC

RGS

Q1Q1

Q2

22

1 4 LSdEEfEQF

EQ

LSdEEfEQF 22

21 4



1-D simulations vs. experimental dataExperimental data courtesy of Columbia University1

1 Rasmussen, A. et al., Proton Scattering off of XMM optics: XMM Mirror and RGS grating samples, XMM project documentRGS-COL-CAL-99009, Nov. 4 1999

1

10

100

0 2 4 6 8 10 12 14

Scatter Angle (degrees)

Flux

(#/c

m2 /s

t/inc

. p+)

Columbia: 1.3 MeV, 1.576deg G4: 1.3 MeV, 1.576deg

RGS Acceptance Range

1

10

100

0 2 4 6 8 10 12 14

Scatter Angle (degrees)

Flux

(#/c

m2 /s

t/inc

. p+)

Columbia: 1.3 MeV, 1.826deg G4: 1.3 MeV, 1.826deg

RGS Acceptance Range

Grating “saw-tooth” surface not modelled correction of ~0.7°

Beam width ~5 mm, simulated beam 1-D


full-scale simulations

Source(restricted isotropic)



SSAT analysis of the XMM baffle

Direct line of sight from the baffle to the focal plane;increases the overall proton transmission efficiency

p



1.E-09

1.E-08

1.E-07

1.E-06

1.E-05

1.E-04

0 5 10 15 20 25 30 35

Source half-angle (deg)

Effi

cien

cy

Scattered 0.1 MeVScattered 0.6 MeVScattered 1.0 MeVDirect Hits 0.1 MeVDirect Hits 0.6 MeVDirect Hits 1.0 MeV


Mirror efficiency

Scattered

Directtransmission




1.E-09

1.E-08

1.E-07

1.E-06

1.E-05

1.E-04

0 5 10 15 20 25 30 35

Source half-angle (deg)

Effi

cien

cy

EPIC 0.1 MeVEPIC 0.6 MeVEPIC 1.0 MeVRGS 0.1 MeVRGS 0.6 MeVRGS 1.0 MeV

EPIC and RGS efficiencies

EPIC

RGS

Variation in Efficiency with Proton Energy at various source half-angles

1.E-09

1.E-08

1.E-07

1.E-06

1.E-05

1.E-04

0.0 0.5 1.0 1.5 2.0 2.5 3.0 3.5

Proton Energy (MeV)

Eff

icie

ncy

EPIC 0.5 degEPIC 1 degEPIC 4 degEPIC 2 degEPIC 10 degEPIC 30 degRGS 0.5 degRGS 1 degRGS 2 degRGS 4 degRGS 10 degRGS 30 deg

EPIC

RGS

-4-2024

-90 -80 -70 -60 -50 -40 -30 -20 -10 0 10

Z (cm)

Y (c

m)

RGS EPIC


Standard Radiation Environment Monitor (SREM)

AluminumTantalumSilicon (detectors)

D1 D2

- Mass (2.5 kg)- Volume (2 l)- Power 2.6 W

e-

p+

e-

Optimised Al-Ta “Sandwich structure”. Original design by Geant3.21 simulations - Electrons > 0.5 MeV

- Protons > 10 MeV- Heavy ions qualitatively


Further miniaturisation underway


FIRSTINTEGRAL

PROBA

International Space Station

Mars Express

Missions with SREM...


Rosetta



Interactions of radiation with biological systems at cellular and DNA level

New Geant4 -based activity in the ESA General Studies Programme Biological and chemical factors... Contractor INFN Genova; network of 20 scientists at INFN, CERN,

ESA, and the Italian National Institute for Cancer Research Heavy ions particularly harmful

Astronaut safety, exobiology

C, Fe, ...



Conclusions ESA has sponsored the development of a set of space-specific

modules Geant4; these will be out by March 2000 Geant4 low-energy electromagnetic models for photons and

electrons down to 250 eV; for protons and ions to ~1 keV; ongoing work also on antiprotons

Complex test case XMM has shown the versatility of the toolkit Being a member in the Geant4 Collaboration offers significant

benefits for ESA Wide user community in space applications foreseen

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ESA Space Environment & Effects Analysis Section

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