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L3+C. Achievements of a L3-based cosmic muon telescope. Pedro Ladron de Guevara Department of Fundamental Physics. High Energy Physics Division CIEMAT-Madrid. NURT-2006 Havane ,Cuba,3-7th April 2006. LEP at CERN (Geneva)

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Nurt 2006 havane cuba 3 7th april 2006

L3+C. Achievements of a L3-based cosmic muon telescope.Pedro Ladron de GuevaraDepartment of Fundamental Physics.High Energy Physics DivisionCIEMAT-Madrid

NURT-2006

Havane ,Cuba,3-7th April 2006


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LEP at CERN (Geneva)

Longitude: 6.020 E; Latitude: 46.250 N; Altitude: 450 m


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Introduction

The succesful LEP detector L3 dedicated to the study of

e+ e- collisions at CERN was equipped along 1997-98 with

additional hardware and software components in order

to measure the muons from cosmic radiation, using the L3 muon

spectrometer. The resulting cosmic muon telescope was named

“L3 + Cosmics” or “L3+C”. It worked from 1999-2000

* A setof plastic scintillators and readout system was installed on top of the magnet to provide a t0 detector.

* Trigger and DAQ electronics independent of L3 to allow both experiments L3 and L3+C to run in parallel.

* GPS timing.

* An Air Shower Detector array of 50 scintillators covering 30 x 54 m2 was installed on top of the L3 building.


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L3+Cosmics

EAS array

* 30 m. of rockonly m

* threshold ~715 GeV

m spectrometer

To measure:

-momentum

-charge

-direction

of the

muons generated in

air showers.

t0 detector (202 m2 scint.)

Magnet: 0.5 T ,1000 m3

Drift chambers

“Trigger” and DAQ

independent of L3

GPS timing

(event time up to 1 ms)

1.2 x 1010 m “triggers” in 312 days of livetime


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Octant structure.

P-chambers measure p in the plane normal to the beam :


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Z-chambers measure positions along the beam


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Schematic view of the meas. on L3+C

One 3-plet at least

1 Scintillator hit

Good running conditions

From good quality tracks on opposite octants:

-momentum resolution

-max. detectable momentum

-scintillator efficiencies

-track selection efficiency

Double octant fit

Single octant fit

Relative momentum

resolution, versus p

at detector level


Physics addressed

Physics addressed

  • Atmospheric muon flux and m+/m-ratio.

  • ap/p in primary spectrum around 1 TeV.

  • Solar flare of 14/July/2000.

  • Point source signals.

  • Anisotropies.

  • Gamma ray bursts.

    Search for exotic events.

    Primary composition in the knee region.

    Very forward physics.

    Meteorological effects of cosmic radiation.

  • ( blue: subjects in progress )

In this talk we will concentrate in the two first subjects


Nurt 2006 havane cuba 3 7th april 2006

The atmospheric muon flux

and the

m+/m- fraction


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The well known origin of atmospheric muon and neutrino fluxes

The dominant process:


Why the atmospheric muon flux is that interesting

Why the atmospheric muon flux is that interesting ?

* Closely related to atmospheric neutrino flux

* m +/ m - => constrains on cosmic primary composition. (…antimatter limits ?)

* constrains for the showering models (i.e. high energy hadron nucleon cross-sections)

* Directionally-related to sidereal point sources at high energies.

* Sensible to middle energies solar emissions (solar flares…) when over threshold.

* …

muons are highly penetrant and

keep track of the primary direction at high energies


Nurt 2006 havane cuba 3 7th april 2006

Atmospheric muons

Current uncertainty

10 - 25 %

F = F . E

-g

primary spectrum

(from 10 GeV to 10 TeV)

0

p

p,K+

X

F

s

p+A

p

10 %

( p )

30 %

( K )

hadronic interactions

(theoretical and experimental)

F

p,K

0 %

decay

(kinematics)

15 % ( m , exp.),

m and n spectrum

F

F

m

n

20 - 30 % (n , theo.)

Use the measured flux of muons toconstrainhadronic interactions

and

atmospheric neutrino flux


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The L3+C suroundings

Simulation of the

L3+C surroundings


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Detector and molasse simulation

The muon input flux at surface, the L3+C environment and the detector response are simulated.

The resulting muons are reconstructed by the same program

used for the data (1.7 x 109 reconstructed Monte Carlo events) 2 x 107 data events after quality cuts for this analysis)

Charge -

Charge +


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Going from the raw data at detector level to spectrum at surface level


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detector level

(measured)

Momentum spectrum

surface level

(computed)

Effective

live time

n = t . D . m

Transformation matrix

E . R . A

migration matrix

matrix of detector efficiencies

function of momentum at the detector level

matrix of geometrical acceptances

function of the surface momentum


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The transformation matrix D = E.R.A

R: migration matrix :The conditional probability of measuring a momentum q p i

given a surface momentum q p j

A: diagonal matrix of geometrical acceptance as a funcion of the surface momentum.

E: diagonal matrix of detector efficiencies as a function of momentum at detector level.

D ij= ei ri SMC(nselij / Ngenj)MC DW

SMC : Surface area used in the MonteCarlo generator.

DW : Solid angle of the zenith bin under study.

ei : Includes the scintillator and trigger efficiency.

ri : Selection efficiency correction.

nselij : The number of selected MonteCarlo events found within a

detector-level momentum bin i, wich were generated within the

momentum bin j at the surface.

Ngenj : Total number of MonteCarlo events generated within this surface

momentum bin.


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Statistical and systematic uncertainties

(momentum scale)

Relative

uncertainties

of the vertical

zenith angle bin

measurements

The individual

contributions

are added in

quadrature.


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Statistical and systematic uncertainties

(m flux)

Relative

uncertainties

of the vertical

zenith angle bin

measurements

The individual

contributions

are added in

quadrature.


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Statistical and systematic uncertainties

(ch. ratio)

Relative

uncertainties

of the vertical

zenith angle bin

measurements

The individual

contributions

are added in

quadrature.


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Total uncertainty:

Obtained by adding the different sources in quadrature.

Muon flux uncertainty:

dominated by :

*The uncertainty of molasse overburden at low momenta.

*The alignment and resolution uncertainty at high momenta.

Minimum is 2.3 % at 150 GeV in the vertical direction.

Vertical charge ratio uncertainty:

Below 2 % up to 100 GeV

Above 100 GeV, rises rapidily with the alignment uncertainties.


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Cross-check of the system


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Let us reconstruct , using L3+C setup

(except the trigger) the L3 collisions with

the same secondary topology as the

cosmic muons, that is:

Z => m+ m-

on the Z peak.


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Analize the LEP events :

e+ e- Z m+m-

 c.m. energy : 91.27 GeV

 mtrackclose to

collision point

 event-time in

coincidence

with the LEP

beam crossing time

pm>27.4 GeV

Absolute cross-section

in excellent agreement

with LEP precision

measurements

Validates our understanding of the detector


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Momentum distribution of the events

e+ e- Z m+m-

+ background

The Monte Carlo

events are normalized

to the LEP luminosity

The arrow indicates

the low-momentum cut

(60% of the beam energy)

The events


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Results


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Measured m flux for zenith angles from 0 0 (bottom) to 58 0 (top)

Inner bars :stat. uncertainty.

Full bars : total uncertainty.

For better visibility, an offset

of 0.05 GeV2 cm-2 s-1 sr-1 was

Added consecutively and lines

are shown to guide the eye.


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Vertical m flux compared with previous results (low energy)


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See Ref [6]

Vertical m flux compared with previous results (all energies)


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Measured m+/ m- charge ratio for zenith angles from 0 0 (bottom) to 58 0 (top)

Inner bars :stat. uncertainty.

Full bars : total uncertainty.

For better visibility, an offset

of 0.05 GeV2 cm-2 s-1 sr-1 was

Added consecutively and lines

are shown to guide the eye.


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Vertical m flux:

* Comparison with low energy experiments gives good overall agreement above 40-50 GeV

* At lower momenta a systematic slope difference seems to be present. Probably due to the

systematic molasse uncertainty

m+/m- ratio:

*The limit is 500 GeV due to the alignment uncertainties.

*In the considered range and within the experimental uncertainties,

it is independent of momentum.

*Mean value in vertical direction:

1.285 + - 0.003(stat.) + - 0.019 (syst.) (chi2/ndf=9.5/11.) to be compared with

1.270 + - 0.003(stat.) + - 0.015 (syst.) (average of all previous measurements)

It is worth noting that the precision of the data of a single L3+C

zenith angle bin is comparable to the combined uncertainty of

all data collected in the past.


Comparison with recent mc muon flux predictions

Comparison with recent MC muon flux predictions

See Ref [7]


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The conection of the atmospheric muon flux and neutrino flux.

* m flux is a good calibration source of the atmospheric n flux

* Honda (Ref [4]) has presented to the 29th ICRC,(Pune,2005)

the comparison of the last measured fluxes from BESS TeV (99)

BESS (2002)and L3+C with the HKKM04 model.

* The ratio between measured fluxes and model show:

- Agreement of < 5% in the 1-30 GeV region.

- Larger disagreement out of this interval.

* Honda et al. modified the DPMJET-III interaction model

(differential cross sections of secondary mesons production)

(only BESS data used under 50 GeV and all data for >50 GeV)

* Better agreement in 1-300 GeV range obtained for m fluxes

* n fluxes more reliable than that of HKKM04 in wider range.


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Conclusions

Using the L3+Cosmics m detector (6.020E, 46.250N) we have determined:

1-the atmospheric m spectrum from 20 GeV to 3 TeV

as a funtion of 8 zenith angles ranging from 00 to 600

with good overall agreement with previous data above 40-50 GeV

for the vertical flux .

2- the ratio m+/m- from 20 GeV to 500 GeV for the same

zenith angles as above.

The mean value in the vertical direction is in perfect

agreement with the average of all the previous data.

3- L3+Cosmics has extended the knowledge of the m momentum spectrum

by a factor ~10 in the momentum range.

4- The precision of the data of a single L3+C zenith angle

bin is comparable to the combined uncertainty of all data

collected in the past.

5-The interest of L3+C data to constrain the MC p,K p-A production

models and the atmospheric n flux calculations as a consequence,

is pointed out.


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THE MOON SHADOW AND THE LIMIT OF ANTIMATTER IN THE

C. R.


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Antiprotons in the CR

Direct measurements up to 50 GeV

Explained by interact.

of the CR with the

interstellar medium.

At higher energies

the detection of

antiprotons should

be very interesting

as it should come from

“exotic sources”.


Nurt 2006 havane cuba 3 7th april 2006

Indirect measurements

m+/m-ratio , (model dependent)

Exists a determination :

(not done by L3+C)

From 1530 TeV the

limit ap/p  ~14 % with 67 % c.l.

and big systematic uncertainties:

-Primary spectrum

-Hadronic interactions at HE


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Moon shadow

CR are blocked by the Moon.

 Deficit of CR when looking at the Moon (Clark,1957)

Size of the deficit  effective ang. resolution.

Position of the deficit  pointing error.

Geomagnetic field :

+ve particles deflected towards the East

-ve particles towards the West

 Ion spectrometer. Urban, ARTEMIS.


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L3+C:

Good angular resolution : (0.22+- 0.04)0 for pm > 100 GeV

Good pointing precision : < 0.20

Precise momentum measurement : Dpm/pm = 7% at 100 GeV

Low pm,min (high rate, large deflection)

Real sensitivity on the earth magnetic field.

THE DEFICIT

Events density vs

angular distance to the

Moon.

a) Background from a

“fake Moon” 1, hour

behind its real position.

b) Using the correct

Moon position.


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Selection :

Good quality events with pm > 50 GeV and angular distance to the Moon <50

Moon zenith < 600

Two energy ranges:

LE (low energy) 65  100 GeV

HE (High energy) > 100 Gev

6.71 x 105 selected evts

What range of primary energies

corresponds to 100 GeV ?

From CORSIKA the peak for protons is 1 TeV

And 4 TeV for He


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The transit of the Moon in the local system.

The angular deflection due to the geom.

field is a function of:

-the direction of incidence

-charge

-momentum

During a transit the deflection depends

mainly on the moon position but weakly

on the momentum.

If we fix p=1 TeV/proton for every position of

the moon we can define a coordinate system

where

QH: Parallel to the deflection

(dispersion due to the geom. field)

QV: Normal to the deflection

(dispersion due to other physical effects)


Nurt 2006 havane cuba 3 7th april 2006

Shadow ( in the deflection coordinates system)


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Model

The density in the plane around the real position of the Moon can be expressed as

x0,y0 : pointing error or directional offset

r = flux(ap)/(flux(p+He)

ux,uy,uz define the background

Nmiss : deficit

f1,f2: parametrizations of the density of the shadow.

  • Hypothesis:

  • -The composition of the primaries around 1 TeV : 75 % protons, 25 % He + others

  • Spectral index of 2.8 similar for matter and antimatter.

  • Functional representation identical for protons and antiprotons.


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Results

Angular resolution:

(0.22 +- 0.04)0 Em>100 GeV

(0.28+-0.08)0 65 GeV< Em < 100 GeV

Pointing error < 0.20

Limit of the ap/p fraction ~1 TeV at 90 % c.l. : 11 %


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Outlook

ALICE, the heavy ions collisions dedicated detector in LHC

( located in the same cavern and magnet than L3+C )

will implement a t0 detector based on plastic scintillators

for the trigger and will use the TPC,TOF and TRD detectors

to detect the atmospheric muons. (ACORDE)


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References

[1] L3+C Collaboration. Adriani et al.,Nucl. Instrum. Methods A488 (2002) 209.

[2] Measurement of the atmospheric spectrum from 20 to 3000 GeV. Phys. Letters B598 (2004) 15-32

[3] T.Hebbeker,C. Timmermans., Astropart. Phys. 18 (2002) 107.

[4] T. Sanuki et al., Atmospheric neutrino and muon fluxes. 29 ICRC, Pune (2005) 00,101-104.

[5] ACORDE, A Cosmic Ray Detector for ALICE. J. Arteaga et al., 29 ICRC, Pune (2005) 00,101-104

[6] Experiments providing an absolute normalization:

Kiel71 : O.C. Allkofer et al., Phys. Lett. B36 (1971) 425.

MARS75 : C.A. Ayre et al., J. Phys. G 1 (1975) 584.

AHM79 : P.J. Green et al., Phys. Rev. D 20(1979) 1598.

CAPRICE : J. Kremer et al., Phys. Rev. Lett. 83 (1999) 4241.

CAPRICE : M. Bozio et al., Phys. Rev. D67 (2003) 072003.

BESS : T. Sanuki et al., Phys. Lett. B541 (2002) 234.

BESS : T.Sanuki et al., Phys. Lett. B581 (2004) 272, Erratum.

BESS-TeV02 : S. Haino et al., astro-ph/0403704

MASS93 : M.P. De Pascuale et al., J. Geophys. Res. 98 (1993) 3501.

[7] MonteCarlo models:

SIBYLL2.1 : R.S. Fletcher et al., Phys. Rev. D50 (1994) 5710.

BARTOL96 : Phys. Rev. D53 (1996) 1314.

QGSJET01 : R. Engel et al., Proc. 26th ICRC(1999) 415.

TARGET2.1 : R. Engel et al., Proc. 27th ICRC(2001) 1381.

DPMJET-III : S. Roesler et al., Proc. 27th ICRC, Hamburg, 1, 439 (2001);

Phys. Rev. D 57, 2889 (1998)

CORT : G. Fiorentini et al., Phys. Lett. B 510 (2001) 173;hep-ph/0103322 v2 27/April/2001

HKKM04 : M. Honda et al., Phys. Rev. D70: 043008 (2004)


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End of presentation

Thankyou !!


Nurt 2006 havane cuba 3 7th april 2006

Extra transparencies


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Some characteristics of the different referenced experiments

Kiel : Solid iron magnet with spark chambers and scintillator counters.

Location: Kiel (Germany) 540 N, 100 E

Altitude : 10 m. asl

MARS : Solid iron magnet + scintillators + flash tubes.

Location: Durham (Great Britain) 540 N, 10 W

Altitude : 70 m. asl

AMH : 2 solid iron magnets + spark chambers +scintillators.

Location: Huston (USA) 290 N, 950 W

Altitude : 10 m. asl

CAPRICE 94 : 4T superconducting magnet spectrometer (balloon) with

proportional and drift chambers, particle identification achieved via

silicon-tungsten calorimeter, RICH and scintillator TOF system.

Location: Lynn Lake (Canada) 56.50 N, 101.00 W

Altitude : 360 m. asl (1000 g/cm2)

Data: July 19-20, 1994.

CAPRICE 97 : Location: Fort Sumner (USA) 34.30 N, 104.10 W

Altitude : 1270 m. asl (887 g/cm2) (balloon)

Data : April 26- May 2, 1997

MASS : Superconducting magnet spectrometer (balloon)

Location: Prince Albert (Canada) 530 N, 1060 W

Altitude: 600 m. asl

BESS : Balloon Borne Experiment with a Superconducting Spectrometer

Altitude: 1030 g/cm2 (1995) , 5-30 g/cm2 (2001)


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Trigger and DAQ in L3 + Cosmics


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Efficiencies

Scintillator efficiencies:

In 50 % of the cases,the muon arrival time is also deduced from the muon chambers.

These tracks are used to determine the scintillator efficiencies (95.6 % -> 94.5 %)

Drift cell efficiency:

The possibility of reconstructing a muon within a single octant is used to scan the

drift-layer performance of the facing octant. (10% of drift cells with efficiency < 80%)

Total effective running time:

Live-time counter and external trigger signals agreed within 0.02 %

Selection efficiency :

Efficiencies e1, e2 in two opposite hemisferes , are computed for data and MC

and compared by means of

r = (e1 x e2)data / (e1 x e2)MC (funcion of charge,momentum and zenith )

8 % inefficiency for the full track selection.


Nurt 2006 havane cuba 3 7th april 2006

Systematic uncertainties

Normalization uncertainties:

Live-time + trigger + scintillator

Uncertainties on the efficiencies of the above give rise to a normalization uncertainty of 0.7 %

Detector acceptance

Uncertainty on detector acceptance is assesed by means of 3 methods:

Comparison of the independent data from 1999 and 2000

Muon flux and charge ratio measured as a function of the azimuthal angle, at large momentum.

Stability of the measured flux and charge ratio with respect to the variation of the selection criteria.

Absolute flux addicional normalization uncertainty :1.7 % -> 3.7 % (depending on the zenith angle)

Charge ratio addicional normalization uncertainty : 1.0 % -> 2.3 %

Magnetic field strenght : momentum scale bias < 0.4 %

Uncertainties on the detector alignment : may induce a constant offset (relative alignment of the

muon chamber octants determined with precision 0.075 -> 0.152 TeV –1

Molasse overburden: Uncertainty on the average rock density of 2 % ->

energy loss uncertainty of 0.4 GeV (in vertical direction)

Momentum scale uncertainties:


Nurt 2006 havane cuba 3 7th april 2006

Detector matrix uncertainty:

Mainly due to statistical uncertainty (MC and data)

Total uncertainty:

Obtained by adding the different sources in quadrature.

Muon flux uncertainty:

dominated by :

*The uncertainty of molasse overburden at low momenta.

*The alignment and resolution uncertainty at high momenta.

Minimum is 2.3 % at 150 GeV in the vertical direction.

Vertical charge ratio uncertainty:

Below 2 % up to 100 GeV

Above 100 GeV, rises rapidily with the alignment uncertainties.


Nurt 2006 havane cuba 3 7th april 2006

L3+C

Device to measure the

momentum

chargeand

angle of

muonscreated in air showhers

Location:

6.020E, 46.250N

Altitude:450 m, 30 munderground

Detector:

t0- detector (202 m2 scint.)

Magnet (0.5 T, 1000 m3)

High precision drift chambers


Nurt 2006 havane cuba 3 7th april 2006

The L3+C experiment:

Muon detector:

* 30 m underground.

* Magnet (0.5 Tesla, 1000 m3

* High precision drift chambers.

* T0 detector (202 m2 of scintillators, 1.8 ns resolution.)

* GPS timing: 1 ms

* Trigger and DAQ: independent of L3.

* Geom. Acceptance : ~200 m2sr

* Energy threshold: Em > 15 GeV

* Mom. Resol.: dp/p = 7.6 % at 100 GeV/c

* Ang. Resol.: dq < 3.5 mrad above 100 GeV/c

Air shower detector:

* 50 scintillators, S=30 x 54 m2

Muon data: 1999-2000: 1.2 1010 triggers, 312 days live-time


Nurt 2006 havane cuba 3 7th april 2006

The fluxes are neither corrected for the altitude of L3+C nor for the atmospheric profile to avoid additional theoretical uncertainties.

Instead, we quote the average atmospheric mass overburden X above L3+C, which was continously measured with balloon flights from close to the experiment to altitudes of over 30 Km, and parametrized as :

A(hb-h) (a-1) , h<11 Km

X(h) =

B e (-h/h0 ) , h>11 Km

Fit to the data yields:

A= 8.078 x 10 –5

B = 1332

h b = 39.17

h0 = 6.370

a = 3.461


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Neutrino flux constraint.

MC study on the neutrino flux constraint. For each interaction model two different

primary fluxes are used, as indicated by the two curves per model.

( From Michael Unger PhD thesis , Humboldt-University, Berlin, 9/February/2004 )


Nurt 2006 havane cuba 3 7th april 2006

Interaction models

TARGET2.1 : Phenomenological model, based on the parametrization of accelerator data

which are extrapolated to the full phase space, energies and target nuclei needed in atmospheric

air showers. Calculations of the neutrino flux based on this model are extensively used to

interpret the data of atmospheric neutrino detectors.

QGSJET01 and SIBYLL2.1 are microscopic models, which predict the hadronic interactions

from first principles and consequently have a much smaller number of free parameters as

TARGET.

* For large momentum transfers between the projectile and target nucleus, the well tested

perturbative QCD theory is applicable.

* For momentum transfers below a few GeV,

-the hadronic interactions are modeled based on the Grivob-Regge theory in case of QGSJET01

-whereas they are described by the production of colored strings in SIBYLL2.1

As no low energy model other than TARGET is implemented in the current version of the

transport code all interactions below a laboratory energy of 100 GeV are handled by this model.


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