The Most Energetic Particles in Nature

(1)

Karl-Heinz Kampert Taipei Colloq, 7.04.2015

The Most Energetic  Particles in Nature

Karl-Heinz Kampert 

University of Wuppertal

ASIAA/CCMS/IAMS/LeCosPA/NTU-Phys Joint Colloquium, April 7, 2015

Area ∝^Grant

(2)

Karl-Heinz Kampert – University Wuppertal 2 Taipei Colloq, 7.04.2015

1 event per m² and sec

γ≈ 2.7 - 3.0

^„ankle“

(1 per km²-year)

Energy Spectrum of Cosmic Rays

log(energy/eV)

log(fl ux)

32 orders of magn.

32 orders of magnitude:

hair

Universe

„Knee“

(1 per m²-year)

(3)

Karl-Heinz Kampert – University Wuppertal 3 Taipei Colloq, 7.04.2015

1 event per m² and sec

γ≈ 2.7 - 3.0

^„ankle“

(1 per km²-year)

log(energy/eV)

log(fl ux)

32 orders of magn. „Knee“

(1 per m²-year)

Balloons Satellite

Air Shower  Exps

<5 m

²

0.1 km

²

<1 m

²

3000 km

²

(4)

Karl-Heinz Kampert 4 Taipei Colloq, 7.04.2015

• Where do they come from?

• What are they made of ?

• How do their accelerators work?

• Is there a maximum limit to their energy ?

• What can they tell us about 

fundamental and particle physics?

Key Questions about 

Ultra High-Energy Cosmic Rays

(5)

Karl-Heinz Kampert – University Wuppertal 5 Taipei Colloq, 7.04.2015 courtesy R. Engel

Particle Energy (eV)

1013 10¹⁴ 10¹⁵ 10¹⁶ 10¹⁷ 10¹⁸ 10¹⁹ 10²⁰

)1.5 eV-1 sr-1 sec-2 J(E) (m2.5 Scaled flux E

1013

1014

1015

1016

1017

1018

1019

(GeV)_pp Equivalent c.m. energy s

102 10³ 10⁴ 10⁵ 10⁶

RHIC (p-p) e-p) HERA (

Tevatron (p-p)

LHC (p-p) ATIC

PROTON RUNJOB

KASCADE (QGSJET 01) KASCADE (SIBYLL 2.1) KASCADE-Grande (prel.) Tibet ASg (SIBYLL 2.1)

HiRes-MIA HiRes I HiRes II

Auger SD 2008

~E^-2.7

~E^-3.1

„Knee“

„Ankle“

Image of non-thermal Universe

„GZK?“

Features of CR spectrum

(6)

1013 10¹⁴ 10¹⁵ 10¹⁶ 10¹⁷ 10¹⁸ 10¹⁹ 10²⁰

1013

1014

1015

1016

1017

1018

1019

102 10³ 10⁴ 10⁵ 10⁶

Tevatron (p-p)

LHC (p-p) ATIC

PROTON RUNJOB

Auger SD 2008

SNR?

Diffusion losses from Galaxis ?

p

....

Fe

SNR ?

Galactic CRs?

Features of CR spectrum

Fe-knee p,He-knee

classical

ankle model

AGN ?

Extragal. CRs?

extragal.

component p

magn. confinement

➠ Emax ~ Z

(7)

1013 10¹⁴ 10¹⁵ 10¹⁶ 10¹⁷ 10¹⁸ 10¹⁹ 10²⁰

1013

1014

1015

1016

1017

1018

1019

102 10³ 10⁴ 10⁵ 10⁶

Tevatron (p-p)

LHC (p-p) ATIC

PROTON RUNJOB

Auger SD 2008

SNR?

Diffusion losses from Galaxis ?

SNR ?

Galactic CRs?

Features of CR spectrum

Fe-knee p,He-knee

AGN ?

Extragal. CRs?

p Fe

?

extragal.

component magn. confinement

➠ Emax ~ Z

(8)

Karl-Heinz Kampert – University Wuppertal Taipei Colloq, 7.04.2015

Lamor radii at 10²⁰ eV compared to Milky-Way

E

₁₈

≤ Z·B

_µG

·R

_kpc

Conjecture:

Extragalactic origin

Size × B-Field needs  to be very large …

Interesting feature:

Can do astronomy with cosmic rays !

10 ²⁰ eV CRs in our Galaxy ?

8

(9)

Cosmic Magnetic Fields

Halo B?

Extra-galactic B < nG ?

γ, ν

weak deflection R_L = kpc Z^-1 (E / EeV) (B / μG)^-1

R_L = Mpc Z^-1 (E / EeV) (B / nG)^-1

strong deflection

Milky way B ~ μG

E > 10¹⁹eV

E < 10¹⁸eV

(E, Z) ⇥ 0.8 10²⁰ eV E

⇥ ⇤ L 10 Mpc

⇤ L_coh 1 Mpc

B 1 nG

⇥

· Z

UHECR Astronomy

(10)

Karl-Heinz Kampert – University Wuppertal

Active Galactic  Nuclei (AGN)

LHC GRB

AGN-Jets

SNR

Colliding Galaxies

Potential Sources of 10

²⁰

eV particles

10 Taipei Colloq, 7.04.2015

Neutron Stars

white dwarfts

Active Galactic Nuclei ?

jets from radio Interplanetary

Space

Galact. disk halo

eV pr oton

galaxies Galactic

Clusters

Size

Magnetic Fieldstrength (Gauß)

1AU

SNR

10¹²

10 ⁶

1

10 ^–6

1km 10 ⁶km 1pc 1kpc 1Mpc

IGM 10 ₂₀

{

LHC

GRB ?

E_max ~ β_s·z·B·L

Fe

Hillas Diagramm

Realistic constraints more severe

• small acceleration efficiency

• synchrotron & adiabatic losses

• interactions in source region

(11)

Cas A 

(3.4 kpc)

Cygnus A

(250 Mpc)

Fornax A

^{(20 Mpc)}

NRAO/AUI

1.4 , 5, & 8.4 GHz

Supernova Remnants Accreting  

Supermassive Black Holes

E < 10

¹⁶

eV

E ~ 10

²⁰

eV ?

Radio Images of Cosmic Accelerators

(12)

The Cosmic Zevatron

courtesy R. Engel

1013 10¹⁴ 10¹⁵ 10¹⁶ 10¹⁷ 10¹⁸ 10¹⁹ 10²⁰

1013

1014

1015

1016

1017

1018

1019

102 10³ 10⁴ 10⁵ 10⁶

Tevatron (p-p)

LHC (p-p) ATIC

PROTON RUNJOB

Auger SD 2008

SNR?

How much would LHC need to   grow to accelerate 10²⁰ eV? 

p-energy LHC

10²⁰ eV protons in LHC would require size of Earth orbit around Sun

(13)

VOLUME 10, ^NUMBER 4 PHYSICAL RK VIEW LKTTKRS ¹⁵ ^I'EBRUARY 196)

cleon-nucleon scattering see, ^for example, M. L. ^Gold-

berger, Q. T. ^Grisaqu, ^S. ^%'. MacDow'ell, and D. Y.

Kong, Phys. Rev. 120, ²²⁵⁰ (1960). ^Other ^methods ^of

calculating phase shifts in terms of scalar ^and vector particle exchanges ^have been considered _by a number of authors. See, for example, R. Bryan, C. ^Dismukes,

and W. Ramsay (to be published).

3R. Blankenbecler ^and M. L. Goldberger, Phys.

Rev. 126, ⁷⁶⁶ (1962); G. F. ^Che~ ^and S. C. Frautschi,

Phys. Rev. Letters 7, ³⁹⁴ (1961);S. Frautschi,

M. Gell-Mann, and F. Zachariasen, Phys. Rev. 126,

2204 (1962); D. ^%'ong, _Phys. Rev. 126, ¹²²⁰ (1962).

4H. Stapp (private communication).

SM. Hull, K. Lassila, H. Ruppel, F. ^McDonald, ^and

G. Breit, Phys. Rev. 122, 1606 (1961).

6C. _de Vries, R. Hofstadter, ^and R. ^Herman, Phys.

Rev. Letters 8, 381 (1962).

7J. _Ball and D. ^%'ong (to be published).

EVIDENCE FOR A PRIMARY COSMIC-HAY PARTICLE WITH ENERGY 10 eV~

John Linsley

Laboratory for Nuclear Science, Massachusetts Institute of Technology, Cambridge, Massachusetts (Received 10 January 1963)

Analysis of a cosmic-ray air shower recorded at the NIT Volcano Ranch station in February

1962 indicates that the total number of particles

in the shower (Serial No. 2-4834) was 5x10'0.

The total energy ^of ^the primary particle ^which

produced the shower was 1.^0x10~ ^eV. ^The ^show-

er was about twice the size of the largest we had

reported previously (No. 1-15832, recorded in

March 1961).'

The existence of cosmic-ray particles having

such a great energy is of importance to astrophys- ics because such particles (believed to be atomic nuclei) have very great magnetic rigidity. It is

believed that the region ⁱⁿ ^which such a particle originates ^must be large ^enough and possess a strong enough magnetic field so ^that REI» _(1/300) x(E/Z), ^{where R} ^is ^the ^radius of the region (cm) and H is the intensity of the magnetic field (gauss).

E is the total energy of the particle _(eV) and Z is its charge. Recent evidence favors the choice Z ⁼ ¹ (proton primaries) for the region of highest

cosmic -ray energies.

'

_For _the _{pr esent} _{event one}

obtains the condition RB» ³ ^x ^10' . ^This ^condition

is not satisfied _by _{our galaxy} (for which RH ~ ⁵

x10", halo included) or ^known objects within it, such as supernovae.

The technique we use has been described else-

where. ' _An _array _of scintillation detectors is used to find the direction (from pulse times) ^and size (from pulse amplitudes) of shower events which satisfy a triggering requirement. In the present case, the direction of the shower was

nearly vertical (zenith angle 10+ 5'). The values of shower density registered at the various points of the array are ^{shown in} Fig. 1. ^It ^can ^be ^ver-

ified _by close inspection of the figure that the

core of the shower must have struck near the

point marked "A," _assuming _only ₍₁₎ _that _shower

particles are distributed symmetrically ^about ^an axis (the "core"), and (2) that the density of par-

ticl.es decreases monotonically with increasing distance from the axis. The observed densities

0.6

KlLOMETERS

FIG. 1. ^Plan ^of the Volcano Ranch array in February 1962. The circles represent 3.^3-m2 scintillation detectors. The numbers near the circles are ^the shower densities (particles/m ₎ registered in this event, No.

2-4834. Point A is the estimated location of the shower core. The circular contours about that point aid in verifying the core location _by inspection.

146

VOLUME 10, ^NUMBER 4 PHYSICAL RK VIEW LKTTKRS ¹⁵ ^I'EBRUARY 196)

cleon-nucleon scattering see, for example, M. L. ^Gold-

berger, Q. T. ^Grisaqu, S. ^%'. MacDow'ell, and D. Y.

Kong, Phys. Rev. 120, ²²⁵⁰ (1960). Other methods of calculating phase shifts in terms of scalar and vector particle exchanges have been considered _by a number of authors. See, for example, R. Bryan, C. Dismukes,

and W. Ramsay (to be published).

3R. Blankenbecler and M. L. Goldberger, Phys.

Rev. 126, ⁷⁶⁶ (1962); G. F. ^Che~ ^and S. C. Frautschi,

Phys. Rev. Letters 7, ³⁹⁴ (1961);S. Frautschi,

M. Gell-Mann, and F. Zachariasen, Phys. Rev. 126,

2204 (1962); D. ^%'ong, Phys. Rev. 126, ¹²²⁰ (1962).

4H. Stapp (private communication).

SM. Hull, K. ^Lassila, H. Ruppel, F. ^McDonald, ^and

G. Breit, Phys. Rev. 122, 1606 (1961).

6C. _de Vries, R. Hofstadter, and R. Herman, Phys.

Rev. Letters 8, ³⁸¹ (1962).

7J. _Ball and D. ^%'ong (to be published).

EVIDENCE FOR A PRIMARY COSMIC-HAY PARTICLE WITH ENERGY 10 eV~

John Linsley

Laboratory for Nuclear Science, Massachusetts Institute of Technology, Cambridge, Massachusetts (Received 10 January 1963)

Analysis of a cosmic-ray air shower recorded at the NIT Volcano Ranch station ⁱⁿ February

1962 indicates that the total number of particles

in the shower (Serial No. 2-4834) was 5x10'0.

The total energy of the primary particle which

produced the shower was 1.^0x10~ eV. The ^show-

er was about twice the size of the largest we had

reported previously (No. 1-15832, recorded in

March 1961).'

The existence of cosmic-ray particles having such a great energy is of importance to astrophys- ics because such particles (believed to be atomic nuclei) have very great ^magnetic rigidity. It is

believed that the region ⁱⁿ which such a particle originates must be large enough and possess a strong enough magnetic field so that REI» (1/300) x(E/Z), ^where ^R ^is ^the ^radius of the region (cm)

and H is the intensity of the magnetic field (gauss).

E is the total energy of the particle (eV) and Z is its charge. Recent evidence favors the choice Z ⁼ ¹ (proton primaries) for ^the region of highest

cosmic -ray energies. ' _For _the _{pr esent} _{event one}

obtains the condition RB»³ ^x ^10' . ^This ^condition

is not satisfied _by our galaxy (for which RH ^~ ⁵

x10", halo included) or known objects within it, such as supernovae.

The technique we use has been described else-

where. ' _An _array _of scintillation detectors is used to find the direction (from pulse times) and

size (from pulse amplitudes) of shower events which satisfy a _triggering requirement. In the present case, ^the ^direction of the shower was nearly vertical (zenith angle 10+ 5'). The values of shower density registered at the various points of the array are shown in Fig. 1. ^It ^can ^be ^ver-

ified by close inspection of the figure that the

core of the shower must have struck near the

point marked "A,"_assuming _only ₍₁₎ _that _shower

particles are distributed symmetrically about an

axis (the "core"), and (2) ^that the density of par-

ticl.es decreases monotonically with increasing distance from the axis. The observed densities

0.6

KlLOMETERS

FIG. 1. Plan of the Volcano Ranch array in February 1962. The circles represent 3.^3-m2 scintillation detectors. The numbers near the circles are the shower densities (particles/m ₎ registered in this event, No.

2-4834. Point A is the estimated location of the shower core. ^The circular contours about that point aid in verifying the core location _by inspection.

146

1962: The First 10

²⁰

eV Event

Volcano Ranch Air Shower  Array, New Mexico

The Most Energetic Particles in Nature