Probing quark matter in compact stars with cosmic rays. Jes Madsen University of Aarhus, Denmark
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1 Probing quark matter in compact stars with cosmic rays Jes Madsen University of Aarhus, Denmark
2 Strangelets in cosmic rays? What are strangelets? Ways to detect a cosmic ray strangelet flux A strangelet search with AMS-02 on the International Space Station A lunar soil strangelet search Strangelets beyond the GZK-cutoff?
3 Ordinary strangelets B=(145 MeV) 4 m S =50, 100, 300 MeV Stable Witten; Farhi & Jaffe Shell-model vs. liquid drop model Bulk E~A Surface tension E~A 2/3 CurvatureE~A 1/3 Madsen, PRD 50 (1994) 3328
4 4 B = (145MeV) vs. (165MeV) 4
5 B = (145MeV) 4 vs. (165MeV) 4 Unstable Stable
6 Color-Flavor Locking Stable = 100MeV BULK STRANGELETS Madsen, PRL 87 (2001)
7 Strangelets have low Z/A Heiselberg, PRD 48 (1993) 1418 [Ordinary strangelets] Madsen, PRL 87 (2001) [CFL] 0.3A 2/3 8A 1/3 Nuclei 0.5A 0.1A
8 From: B. Monreal (nucl-ex/ )
9 Detecting strangelets at GV Find low Z/A cosmic rays with high precision equipment in space => AMS-02
10
11 AMS-02 Collaboration USA A&M FLORIDA UNIV. JOHNS HOPKINS UNIV. MIT - CAMBRIDGE NASA GODDARD SPACE FLIGHT CENTER NASA JOHNSON SPACE CENTER UNIV. OF MARYLAND-DEPRT OF PHYSICS UNIV. OF MARYLAND-E.W.S. S.CENTER YALE UNIV. - NEW HAVEN MEXICO UNAM Y _1Commitment NETHERLANDS ESA-ESTEC NIKHEF NLR FRANCE GAM MONTPELLIER LAPP ANNECY LPSC GRENOBLE SPAIN CIEMAT - MADRID I.A.C. CANARIAS. PORTUGAL LAB. OF INSTRUM. LISBON DENMARK UNIV. OF AARHUS FINLAND HELSINKI UNIV. UNIV. OF TURKU ITALY ASI CARSO TRIESTE IROE FLORENCE INFN & UNIV. OF BOLOGNA INFN & UNIV. OF MILANO INFN & UNIV. OF PERUGIA INFN & UNIV. OF PISA INFN & UNIV. OF ROMA INFN & UNIV. OF SIENA GERMANY RWTH-I RWTH-III MAX-PLANK INST. UNIV. OF KARLSRUHE ROMANIA ISS UNIV. OF BUCHAREST SWITZERLAND ETH-ZURICH UNIV. OF GENEVA RUSSIA I.K.I. ITEP KURCHATOV INST. MOSCOW STATE UNIV. CHINA BISEE (Beijing) IEE (Beijing) IHEP (Beijing) SJTU (Shanghai) SEU (Nanjing) SYSU (Guangzhou) SDU (Jinan) 16 Countries, 56 Institutes, 500 Physicists ~ 95% of AMS is constructed in Europe and Asia KOREA EWHA KYUNGPOOK NAT.UNIV. TAIWAN ACAD. SINICA (Taiwan) CSIST (Taiwan) NCU (Chung Li) NCKU (Tainan) NCTU (Hsinchu) NSPO (Hsinchu)
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15 Debris Debris
16 Alpha Magnetic Spectrometer AMS-02 International Space Station (or longer) PURPOSE Cosmic rays Antimatter (anti-he) Dark matter Strangelets Superconducting magnet technology
17 The AMS superconducting magnet coils are fully assembled: Volume 35 cu. ft., Field 8,600 Gauss, Weight 2 tons
18
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20 Choutko (MIT)
21 Strangelets from strange star binary collisions 1 binary neutron star collision per 10,000 years in our Galaxy Release of 10-6 solar masses per collision Basic assumptions: SQM absolutely stable! All mass released as strangelets with mass A (fluxes for mass A give lower limit of flux if mass spectrum of masses below A)
22 Strangelet propagation Acceleration in supernova shocks etc Source-flux powerlaw in rigidity Diffusion in galactic magnetic field Energy loss from ionization of interstellar medium and pion production Spallation from collision with nuclei Escape from galaxy Reacceleration from passing shocks
23 Cosmic strangelet flux Z=8, A=138 [CFL] Flux (per [year GV sqm sterad]) Source Interstellar Solar System Madsen (2005) Phys.Rev. D 71, Rigidity (GV)
24 Total CFL-strangelet flux Total flux (per [year sqm sterad]) No geomagnetic cutoff Interstellar Solar System Madsen (2005) Phys.Rev. D 71, Z
25 Total CFL-strangelet flux Total flux (per [year sqm sterad]) No geomagnetic cutoff Interstellar Solar System Madsen (2005) Phys.Rev. D 71, A Mass number
26 Detecting strangelets at 100 MeV Find low Z/A nuclei in lunar dust with high precision accelerator mass spectrometer => Lunar Soil Strangelet Search
27 The Moon as a strangelet detector
28
29 Wright Nuclear Structure Lab Yale LSSS-collaboration: Sandweiss, Majka, Finch, Ashenfelter, Beausang, Casten, Chikanian, Han, Heinz, Parker, Emmet, Baris (Yale) Fisher, Monreal (MIT) Madsen (Århus)
30 Background Ions in E-dE
31 First run March 2005
32 Cronin, Gaisser & Swordy (1997)
33 Strangelets could also explain Ultra-High Energy Cosmic Rays Madsen & Larsen, PRL 90 (2003) Avoids the acceleration problem of ordinary UHECR candidates (HIGH Z) 2. Avoids the GZK cut-off from interaction with 2.7K cosmic microwave background (HIGH A)
34 Eliminating the GZK-cutoff a) Photo-pion production cut-off at E γ Amp eva photo-pion π b) Photo-disintegration at E γ Amp eva photo-dis dis c) Photo-pair-production above E γ Amp eva photo-pair pair γ dis 10MeV / 2 1 de / dt Z A small for low Z / γ γ π A mπ / E2. 7K E 2. 7K pair 2me / E2. 7K
35 Conclusions Strangelets have low Z/A CFL and non-cfl strangelets differ wrt. Z Experimental verification/falsification of Strangelet existence Realistic from AMS-02 [2008-?] Possible from lunar soil search [2005] (A,Z)-relation (CFL or ordinary) Optimistic, but not impossible from AMS-02 or lunar soil search Possible explanation of UHECR s
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