rhic physics through the eyes of phobos
DESCRIPTION
Moriond, March 2003. RHIC Physics Through the Eyes of PHOBOS. Wit Busza MIT. Relativistic Heavy Ion Collider. Why Collide Heavy Ions?. From Frank Wilczek. time. s NN = 130 GeV. Gold. Gold. UA1, 900 GeV. anti-proton. proton. - PowerPoint PPT PresentationTRANSCRIPT
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RHIC Physics Through the Eyes of PHOBOS
Wit Busza
MIT
Moriond, March 2003
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Relativistic Heavy Ion Collider
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time
From Frank Wilczek
Why Collide Heavy Ions?
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proton anti-proton
UA1, 900 GeV
Gold Gold
sNN = 130 GeV
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Goal of Relativistic Heavy Ion Physics is to Obtain a Better Understanding of the Solutions of the QCD Lagrangian:
• QCD Phase Diagram• Properties of QGP• Mechanism of Particle Production • Structure and Interactions of Relativistic
Hadrons & Nuclei
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Spectator Nucleons
Participating Nucleons
Npart= 7
Ncoll.= 10
Nquarks +gluons = ?
Ninelastic= 1
In calculating Npart or Ncoll
taken to be nucleon-nucleon inelastic cross-section. A priori no reason for this choice other than that it seems to give a useful parameterization. inel ~ (R1+R2)2 ~ (A1
1/3 + A21/3)2 ~ A2/3
Npart ~ A2/3(A11/3+ A2
1/3) ~ A
Ncoll ~ A2/3(A11/3 * A2
1/3) ~ A4/3
What Are the Correct Variables When Looking at AA Collisions?
Will the following be equivalent to the above?
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pA multiplicities were found to be proportional to Npart
Busza et al., PRL 41(1978).285
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In no rest frame is this picture correct
In rest frame of one nucleus:
Soft components overlap, “gluon saturation effects”, shadowing etc.
The use and relevance of Npart is far from obvious when the collision is viewed from different frames of reference
In rest frame of the center of mass of the system:
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19.6 GeV 130 GeV 200 GeVPHOBOS PHOBOS PHOBOS
Central Collisions
Peripheral Collisions
dNd
1. Is there an interesting state created in high energy hadronic (in particular AA) collisions?
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Initially released energy density >5GeV/fm3
Note: energy density inside proton ≈ 0. 5GeV/fm3
1=1−=
o45
1000~all
d
dN⎟⎟⎠
⎞⎜⎜⎝
⎛
GeVE 1~
32 200~)1(~ fmfmRπ
Total energy released ~2000GeVMax. initial overlap volume
Evidence that shortly after the collision a high energy density* is created
Nu
mb e
r o f
Pa r
t icl
es P
rod
u ce d
at
y=0
Energy of Collision
* Strictly speaking it is the energy released in the transverse direction per unit volume
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K–/K+
p/p
Rati
o o
f an
tim
att
er
to m
att
er
A+A central collisions
Energy of collision
Evidence that at y≈0 this high energy density state has the quantum numbers of the vacuum
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• Jets seen in peripheral Au+Au and p+p
• Azimuthal correlations– Small angle ( ~ 0)– Back-to-Back ( ~ p)
Peripheral Au+Au data
Evidence for interactions with the created state
Central Au+Au data
• Disappearance of back-to-back correlations in central Au+Au
• Away-side particles absorbed or scattered in medium
D. Hardtke
QM ‘02
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Azimuthal Angular Distributions
“head on” view of colliding nuclei
Also, PHOBOS sees very few low Pt particles
All this is direct evidence of collective effects
Peripheral Central
Phobos data for 130 and 200 GeV
Evidence that the created state has a high pressure
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Preliminary v2200
Final v2130
PHOBOS Au+Au
v 2
200 GeV
130 GeV
<Npart>~190 130 GeV result: nucl-ex/0205021, submitted to PRL
PHOBOS preliminary
h+ + h-
200 GeV Au+Au
0<<1.5
(top 55%)
v 2
17% scale error
Elliptic Flow
Evidence that most of the action ends very quickly after the collision
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Evidence that the system may reach some kind of equilibriuim
NA49, Phys Lett B459 (1999) 679NA49, PRL 86 (2001) 1965
From Gunther Roland/MIT
Event by Event Fluctuations
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Further evidence that it may be reaching statistical equilibrium
STAR Preliminary
Gene Van Buren.QM’02
Particle ratios compared to statistical model
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2. There are remarkable similarities between e+e-, pp & AA collisions
Is this evidence that dynamics are dominated by the initial state interactions?
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19.6 GeV 130 GeV 200 GeVPHOBOS PHOBOS PHOBOS
Central Collisions
Peripheral Collisions
dNd
Collision viewed in rest frame of CM:
Limiting fragmentation
Collision viewed in rest frame of one nucleus:
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)GeV(s24 31 5345 63
2-4
5-9
10-
14
15-
19
20-
24
Tot
al o
bser
ved
mul
tiplic
ity
d
d n
n
1
W. Thome et al.,Nucl. Phys. B129(1977) 365.
ISR data Proton+Antiproton
UA5
900 GeV
546 GeV
200 GeV
53 GeV
0-2-4-6-ybeam
0
1
2
3
4
Limiting fragmentation:
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Au+Au
(preliminary)
)/exp( sBsch CAN αα=
Nu
mb e
r o f
Pa r
t icl
es P
rod
u ce d
Energy of Collision
e+e-
Au+Au
Eskola, QM ’01
dN/d||
e+e-Amazing similarity of AA and e+e-
From P. Steinberg
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200GeV 130GeV
19.6GeV (PRELIMINARY)
Au+Au yields normalized to corresponding pp value for all three
energies
pp Errors from Au+Au only
PHOBOS Au+Au
19.6 GeVpreliminary
130 GeV
200 GeV
e.g. impact parameter dependence of the number of particles produced at the center of mass of the collision
PRC 65 (2002) 061901R
pp
Slow quark
Fast quark
3. Some results inconsistent with naïve expectations:
Data inconsistent with the following picture:
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“X-Ray” of Medium Using Jets
Leading Particle
Hadrons
q
q
Hadrons
Leading Particle
Hadrons
q
q
Hadrons
Leading Particle
Leading Particle
4. Direct study of the properties of the produced state
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Charged Hadron Spectra
Preliminary sNN = 200 GeV
Preliminary sNN = 200 GeV
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Rel
ativ
e Y
ield
per
par
tici
pant
Submitted to Phys.Lett.
Fast quark
Particle Production at high Pt
Cronin effect data
PHOBOS
pA
AuAu 200GeV
AuAuNcollscaling
Ncollscaling
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“Quenching” of leading partons in pA collisions?
W. Busza Nucl.Phys. A544 (1992) 49c
Eichten et al.
Baron et al.
Skupic et al.
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Summary• pp, pA, AA collisions are magnificent laboratories
for the study of QCD
• No doubt a very high energy density creates a fascinating medium. If it equilibrates, it does so quickly. If it is the QGP, the transition is almost certainly a cross-over
• Main difficulty in interpretation of data is the separation of the initial and final state interactions
• Data continues to surprise us– Smoothness of data with energy – Jet quenching– Similarity of AA with e+ e-
– Why approx. Nparticipant scaling, even at high Pt?
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Collaboration (Jan 2003)
Birger Back, Mark Baker, Maarten Ballintijn, Donald Barton, Russell Betts, Abigail Bickley,
Richard Bindel, Andrzej Budzanowski, Wit Busza (Spokesperson), Alan Carroll, Patrick Decowski,
Edmundo Garcia, Nigel George, Kristjan Gulbrandsen, Stephen Gushue, Clive Halliwell,
Joshua Hamblen, George Heintzelman, Conor Henderson, David Hofman, Richard Hollis,
Roman Holynski, Burt Holzman, Aneta Iordanova, Erik Johnson, Jay Kane, Judith Katzy, Nazim
Khan, Wojtek Kucewicz, Piotr Kulinich, Chia Ming Kuo, Jang Woo Lee, Willis Lin, Steven Manly,
Don McLeod, Jerzy Michalowski, Alice Mignerey, Gerrit van Nieuwenhuizen, Rachid Nouicer,
Andrzej Olszewski, Robert Pak, Inkyu Park, Heinz Pernegger, Corey Reed, Louis Remsberg,
Michael Reuter,
Christof Roland, Gunther Roland, Leslie Rosenberg, Joe Sagerer, Pradeep Sarin, Pawel Sawicki,
Wojtek Skulski, Stephen Steadman, Peter Steinberg, George Stephans, Marek Stodulski,
Andrei Sukhanov, Jaw-Luen Tang, Ray Teng, Marguerite Belt Tonjes, Adam Trzupek, Carla Vale,
Gábor Veres, Robin Verdier, Bernard Wadsworth, Frank Wolfs, Barbara Wosiek, Krzysztof
Wozniak, Alan Wuosmaa, Bolek Wyslouch
ARGONNE NATIONAL LABORATORY BROOKHAVEN NATIONAL LABORATORYINSTITUTE OF NUCLEAR PHYSICS, KRAKOW MASSACHUSETTS INSTITUTE OF TECHNOLOGYNATIONAL CENTRAL UNIVERSITY, TAIWAN UNIVERSITY OF ILLINOIS AT CHICAGO
UNIVERSITY OF MARYLAND UNIVERSITY OF ROCHESTER