13 january, 2005seminar at ucsc 1 up-to-date cosmic p-ism interaction modeling and “anomalies”...

13 January, 2005 Seminar at UCSC 1

Up-to-date Cosmic p-ISM Interaction Modeling and“Anomalies” in -Rays, Positrons, and Anti-Protons

13 January, 2005Tune Kamae (SLAC)

(in collaboration with colleagues at SLAC)

Plan of this Talk

Galactic diffuse -ray emission“GeV Excess” in the EGRET spectrum

Recent work on p-ISM interactionWhat are new in this work

Model A with diff. process and scaling violationGeV Excess explained?

Anomalies in e+ and p-bar explained?Conclusion and future Prospects


Galactic Diffuse -ray Emission: COS-B Observation - First glimpse into cosmic ray interaction with ISM -

Galactic diffuse emission by pp->pi0, bremsstrahlung, and inverse-Compton scattering predicted by Ginzburg, Hayakawa and others in 1960’s.

Galactic Center

Vela pulsar

Crab pulsar

Geminga pulsar

Cygnus region

Local structure(Ophiuchus)


Gal. Diffuse Emission, Accel. Sites, and CR Propagation- Interplay of CR, ISM and B-field -

Escaping electron

Galactic Halo

Galactic Ridge

Trapped proton

Trapped electron Brems. (diffuse)

IC by elect(diff)

0()(conf)

IC at accel site

(conf)

Escaping proton

0production (direct + decay)

in GMC

Accel. sites (SNR, pulsar)Star light

(rad. field)

Earth

Synch. rad. at

accel site(confined)

0()(diff)


Galactic Diffuse -ray: Modeling of pp Interaction - Early models for pp -> p0 inclusive production -

Data from Fermi Lab

Earlier models need to be re-examined with data from ISR, CERN-SPS, and Fermi Lab and measurements.

Galactic diffuse emission by pp->pi0: Predicted by S. Hayakawa, Ginzburg, et al.Early models of PP->pi0 for astrophysical applications: Stecker, Stephens & Badwar, and Dermer


Galactic Diffuse -ray: EGRET Observation - Intensity Map -

Galactic Ridge


Galactic Diffuse -ray: Diffuse Emission - 271 point-sources subtracted -

E=70-100MeV

E=100-150MeV

E=150-300MeV

Av. Intensity of this region


Galactic Diffuse -Ray: EGRET GeV Excess

Hunter et al. 1997

Excess

6<b<10

2<b<6

-2<b<2

-6<b<-2

Data

Scaling model prediction

Scaling model prediction

Data

dN/dE

E[MeV]

E2dN/dE

E[MeV]


ISM-Bound Emission: No.1/2 - Longitudinal distribution predicted by Strong, Moskalenko, & Reimer -

GC

GC

GCGC

GC GC

E=100-150MeV E=150-300MeV E=300-500MeV

E=500-1000MeV E=1-2GeV E=2-4GeV


ISM-Bound Emission: No.2/2 - Glat Distr for 3 Glon Regions (-74~-34,-30~30,34~74) -

l=-74~-34 l=-30~-30 l=34~-74Deconvoled Deconvoled Deconvoled

Thickness of the measured Galactic disk: independent of E and Glon

Galactic Plane

Galactic Plane

Galactic Plane

Intensity map from the EGRET archive

New intensity map by T.K. et al to be published


Galactic Diffuse -ray: Modern Simulation Studies No.1/2- PP 0 -ray in SNR and Galactic Ridge -

Proton’s power-law

index = 2.0

Proton’spower-lawindex =2.0,2.25,2.5

Scaling law

Scaling law

IsobarModel (Dermer)

IsobarModel (Dermer)


Galactic Diffuse -ray: Modern Simulation Studies No.2/2- Run with Early Version of Pythia -

M. Mori simulated pp > 0 > -ray using HADRIN and PYTHIA in 1997 and concluded that their prediction is similar to the scaling model predictions.

Index of protons~2.73


What Are New in The Present Work?

1. Diffractive process (“Renormalized”) in the cosmic PP interactions.2. Scaling Violation (Pythia with CDF Tune A) in the cosmic PP interactions.

A. All secondary particle fluxes will increase in the GeV-TeV range. B. Diffraction dissociation favors positively charged secondary particles.

Three “anomalies” may be explained by diffractive process and scaling violation:• GeV Excess in Galactic -ray spectrum • p-bar flux at Earth• e+ spectrum at Earth

Parameterized e e+, , -bar, p-bar inclusive spectra for 0.5 GeV<Tp<512 TeV

Programs used: • Pythia 6.2 (with CDF Tune A),• U. W.-Milwaukee parameterization of the Stephens-Badhwar model [coded by TK] • Diffraction Dissociation model (DiffDissocSimNew.py) [coded by TK]


Our Model A and Model B

Model A (the most-updated and our preferred model): tot(pp)=el+inel(non-diff)+inel(diffractive)

Non-diffractive inelastic interaction:• Tp>=62.5GeV: Pythia 6.2 with “Scaling violation” through “multiple interaction” (CDF TuneA included in Pythia 6.2)• Tp<62.5GeV: Parameterized version of the Stephens-Badhwar Model (by a group at U. of Wisconsin at Milwaukee) (same for Model B)

Diffraction process: (DiffDissocSimNew.py)• “Renormalized” diffraction model by K. Goulianos 1995

Model B (used for confirmation: no scaling violation in the non-diff part nor no “renormalization” in diff part)

Non-diffractive inelastic interaction:• Tp>=62.5GeV: Pythia 6.1 without “Scaling violation”


PP Cross Sections: Scaling Model (Model B) - Particle Physics in 1960-1970 -


PP Cross Sections: Our Model A - Scaling Violation & Renormalized Model of Diffraction -

Scaling ModelOur Model A


Pythia with Scaling Choice with Model B Cross-Section- Inclusive gamma-ray cross-section -

Tp=512TeV

Tp=256TeV

Tp=62.5GeV

Model B


Pythia with Scaling Violation and Model A Cross-Section- Inclusive gamma-ray cross-section -

Tp=512TeV

Tp=256TeV

Tp=62.5GeV


Low Energy PP Interaction: Stephen & Badhwar Model No.1/2

S. R. Blattnig et al., “Parametrizations of Inclusive Cross-Sections for Pion Production in Proton Proton Collisions“, Phys. Rev. D62, 094030 (2000)

Common to Model A and Model B except for cross-section


Low Energy PP Interaction: Stephen & Badhwar Model No.2/2- Gamma-Ray Spectrum -

S. R. Blattnig et al., “Parametrizations of Inclusive Cross-Sections for Pion Production in Proton Proton Collisions“, Phys. Rev. D62, 094030 (2000)

Common to Model A and Model B except for cross-section


Diffractive Process: No.1/3- Monte Calro Simulator “DiffDissocSimNew.py”-

Diffractive Processes

Double-Diff. Proc.

Single-Diff. Proc.Projectile-Diff. Proc.

Target-Diff. Proc.

Mass2 of “excited fireball”

Mass2 of “excited fireball” Mass2 of “excited fireball”

Target region

Target region Target region

Projectile region

Projectile region

Projectile region


Diffractive Process: No.2/3- Monte Calro Simulator “DiffDissocSimNew.py”-

Double-Diff. Proc.

pLab of the projectile fireball

pLab of the target fireball

Nch of the projectile fireball

Nch of the target fireball


Diffractive Process No.3/3- Double peaked spectra with low multiplicity -


Relative -Ray Yields: Model A and Model B- Non-Diffractive Process -

Model A = 1.65 x Model B


Relative g-Ray Yields: Model A Diff and Non-Diff- Importance of Diffractive Process -

Diff. contributessignificantly here.


Verification of Model A: No.1/2- Charged Multiplicity Distribution -

Scaling Model

Model A

UA5 Data


Verification of Model A: No.2/2- Pi-zero Multiplicity -

Scaling Model

Model A


Cosmic Proton Spectrum in Galactic Ridge: Galprop No.1/2- Galaxy simulator by Strong and Moskalenko -

Moskalenko, Strong, Ormes & PotgieterApJ, 565, 280 (2002)

Local Intersteller Spectrum (LIS)

LIS

LIS

Spectrum near Earth (Near Earth)

Modulation by Solar B-fieldand Solar Wind

Near Earth

Near Earth

Particleinteractionmodeling


Cosmic Proton Spectrum in Galactic Ridge: Galprop No.2/2- Galaxy simulator by Strong and Moskalenko -

Slightly harder “injection spectrum” at cosmic-ray sources: our Trial4GR spectrum

Boron/Carbonratio

Positron spectrum p-bar spectrum

LIS under-predict


Galactic Diffuse -ray Spectrum for Ind=2, LIS and Trial4GR

Prediction of Scaling Models

Prediction of Model A

Scaling Models Model A

Model A predicts:1) a harder -ray spectrum (diffractive process)2) a higher flux (rising non-diff. cross-sec. and scaling violation)than scaling models


GeV Excess Explained ? No.1/2

EGRET Intensity inL=(-30,30) B=(-5,5)

Model A (LIS)

SMR04 (LIS)

Gamma-rays from pp 0

Model B (LIS)


GeV Excess Explained? No.2/2

Scaling Models

EGRET

Model A (LIS)

Model A (Trial4GR)

Explains about 50%of the Excess with LIS.

Explains the Excess fully with Trial4GR.

Our 0 Brems ICGalprop, LIS)


Anomalies in e+ and p-bar ? No.1/2

de Boer et al. 2003

Neutralino decay to -ray? Neutralino decay to p-bar?


Anomalies in e+ and p-bar ? No.2/2

de Boer et al. 2003Measurement by HEAT collaboration(e+ spectrum by a series of balloon exp.)


Model A Prediction on p-bar Spectrum

Exp. data

Scaling modelwith LIS

Model A vs. Model B


Model A Prediction on Positrons Spectrum

Diffractive process favorse+ over e-

e+

e-

Non-Diffractive process dominates overall spectrum


Parameterization of pp > Inclusive Cross-Sections

Non-diffractivered: fit to simulated datablue: parameterization

Definition of P0-P8: x = log10(Tp) 0.000488<Tp< 512.0TeV[0]*exp(-[1]*( x-[3] + [2]*(x-[3])**2)**2) + [4]*exp(-[5]*( x-[8] + [6]*(x-[8])**2 + [7]*(x-[8])**3)**2)

d( incl)/dlogE = Sum of the following two “skewed” Gaussians [0]*exp(-[1]*((x-[2])/(1.0+[3]*(x-[2])))**2) [4]*exp(-[5]*((x-[6])/(1.0+[7]*(x-[6])))**2)

Diffractive dissoc.red: fit to simulated datablue: parameterization


Parameterization of pp > e Inclusive Cross-Sections

Diffractive dissoc.red: parameterization for e+blue: parameterization for e

Non-diffractivered: parameterization for e+blue: parameterization for e

Definition of P0-P8: x = log10(Tp) 0.000488<Tp< 512.0TeV[0]*exp(-[1]*( x-[3] + [2]*(x-[3])**2)**2) + [4]*exp(-[5]*( x-[8] + [6]*(x-[8])**2 + [7]*(x-[8])**3)**2)

d( incl)/dlogE = Sum of the following two “skewed” Gaussians [0]*exp(-[1]*((x-[2])/(1.0+[3]*(x-[2])))**2) [4]*exp(-[5]*((x-[6])/(1.0+[7]*(x-[6])))**2)


Conclusion and Prospects for GLAST

1. Accurate modeling of p()-ISM interaction is likely to explain the GeV Excess with minor modification in the cosmic proton () spectrum.

2. We expect a higher anti-proton flux for Model A (rising and scaling violation).

3. Excess of e+ flux over e expected for E > 5 GeV by the diffractive process.

4. With much improved -ray data from GLAST and e+/p-bar data from PAMELA, we can map the baryonic matter distribution in the Galaxy accurately.

5. We will incorporate our Model A to Galprop and make a very reliable model of Galaxy in near future.


What can we do beyond GLAST?

1. Parameterize angular distri. of secondaries >> Simulate AGN jets >> -rays from filaments in SNR

2. Include multiple Pomeron Ex. (in diff. dissoc.), mini-jets (multiple parton int.) and nuclear effects >> Calibrate AGASA/Hires/Auger and study UHE

3. New particle physics? >> Study the first UHE interaction in the upper atmosphere

13 january, 2005seminar at ucsc 1 up-to-date cosmic p-ism interaction modeling and “anomalies”...

Documents

regiongalactic diffuse

ism galactic diffuse

mori simulated pp p0

cosmic ray interaction

cosmic pp interactions

early models of pp

ismbound emission

measured galactic disk