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(In)direct signatures for ~ axions

(In)direct signatures for ~ axions. K. Zioutas Physics Department University of Patras & CERN  ILIAS–axions WG HEP 2006 University of Ioannina, Greece 16/4/2006. mimic CAST.  (in)direct axion-signals ?.

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(In)direct signatures for ~ axions

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  1. (In)direct signatures for ~axions K. Zioutas Physics Department University of Patras & CERN ILIAS–axions WG HEP 2006 University of Ioannina, Greece 16/4/2006

  2. mimic CAST  (in)direct axion-signals?

  3. Αστροφυσικά σήματασε συνεργασία με: K. Dennerl / MPE L. Di Lella / CERN M. Grande / RAL-UK Th. Hackman / UH-FI D.H.H. Hoffmann / TU-Darmstadt J. Huovelin / UH-FI J. Jacoby / U. Frankfurt B. Lakic / RBI - Zagreb S. Orlando / INAF-Palermo A. Ortiz/ U. Barcelona Th. Papaevangelou / CERN Y. Semertzidis / BNL-USA Sp. Tzamarias / HOU-GR O. Vilhu / UH-FI κ.π.ά. Indirect signatures for axion(-like) particlesTAUP2005 astro-ph/200603507 K. Zioutas, K. Dennerl, M. Grande, D.H.H. Hoffmann, J. Huovelin,B. Lakic, S. Orlando, A. Ortiz, Th. Papaevangelou, Y. Semertzidis, Sp. Tzamarias, O. Vilhu

  4. Power-law index n of Lx ~ Bn=(time) YOHKOH / XRT The relation between the solar soft X-ray flux (below ~4.4keV) …and B can be approximated by a power law with an averaged index close to2. Benevolenskaya, Kosovichev, Lemen, Scherrer, Slater ApJ. 571 (2002) L181 Note:axion-to-photon oscillation ∝ B2 e.g., inCAST D.H.H. Hoffmann, K. Z., Nucl. Phys. B Suppl. 151 (2006) 359 11 years solar cycle? 

  5. The long-term evolution of AR 7978(S10o) Yohkoh / SXT Lx  Lx B1.94±.12 X-ray flux outside flaring times in AR7978 ● increased steeply @flux emergence - - - - -+ - - - - - decreased @decay phase ~ filter independent Eγ < 4 keV B [Gauss] <X-ray flux> / (cm2 -AR7978)vs. magnetic field <B>(=total magnetic flux / ARsurface). Solid line: the linear fit; dotted lines: the 3σ error in the slope of the solid curve. Only the decaying phase (diamonds) is included in the fit  July-Nov. 1996 • The only sizable and long-lived AR on the solar disk @ 5 solar rotations  it produced 3 slow CMEs + 3 major flares L. van Driel-Gesztelyi, P. Démoulin, C.H. Mandrini, L. Harra, J.A. Klimchuk, ApJ. 586 (2003) 579 TAUP2005

  6. KZ et al., astro-ph/200603507 S.K. Solanki, A.&A. Rev. 11 (2003) 153

  7. Solar temperature distribution ↛ 2nd Law of Thermodynamics?solar corona problem Grotrian(1939)  The enigma of coronal heating represents one of the most challenging problems in astrophysics at the present time. E. R. Priest, D. W. Longcope, J. Heyvaerts, ApJ. 624(2005)1057

  8. Stellar observations + theory on stellar evolution ↛ stars might possess atmospheres … that produce X-rays. L.W. Acton, Magnetodynamic Phenomena in the Solar Atm. (1996) 3  The magnetic field plays a crucial role in heating the solar corona (this has been known for many years) the exactenergy release mechanism(s)is(are) still unknown.  the process by which it is converted into heat and other forms remainsa nagging unsolved problem. Signal for Axions? K. Galsgaard, C.E. Parnell, A.& A. 439 (August 2005) 335 R.B. Dahlburg, J.A. Klimchuk, S.K. Antiochos, ApJ. 622 (2005) 1191

  9. RHESSI Major Events ****************************2005************************** October 18, 09:00 UT RHESSI was again put into drift mode to view the x-ray emission of the quiet Sun "out of the corner of its eye". This mode began at the time noted above. RHESSI was commanded back to the Sun at 06:10 UT on October 28, and arrived shortly after 08:00 UT on that day. The Sun was very quiet during this time, but anyone wishing to analyze data within that interval should contact the instrument team.  10 days July 19, 06:00 UT At this time, RHESSI was put in a new mode that let it drift up to 1 degree away from the Sun and slewed back, repeatedly. The purpose of this mode was to study the x-ray emission of the quiet Sun (the Sun was extremely quiet beginning at this time). RHESSI returned to normal operations at around 04:00 UT on July 26. If you wish to analyze any flares during this week, please contact the instrument team.  7 days

  10. SMART:orbiting X-ray detectorsdark moon large volume + backgr. Sun collaboration with Observatory UH-FI RAL-UK Search for massive ~axions spontaneous radiative decays aγγ

  11. X-ray mysteries: • Class 0 protostar  origin of X-rays (<10 keV): • (10-100 kyears) matter is falling 10x faster? • K. Hamaguchi et al., ApJ. 623 (2005) 291 • Similar-to-Sun logic=wrong  • Galactic Center origin of diffuse X-rays? • too hot (~ 90MK) to be a gravitationally • bound plasma! •  how to produceit? • Clusters of Galaxies “strong evidence of some thing wrong” • “physical mechanism for the energy • (or the entropy) excess? “ • “some homogeneous process heats • the gas” • P. Tozzi, astro-ph/0602072 • XRBradiation origin?

  12. V Q 4.2σ 9σ expected S-Z expected S-Z W X-rays observ. Hot gas properties 31 co-added WMAP cluster fields  expected S-Z effect 4x bigger less e-  Radiative decay of massive particles,  e.g. axions of the KK-type  to reconcile contradiction R. Lieu, J.P.D. Mittaz, M. Bonamente, S-N.Zhang, astro-ph/200510160 2.3σ expected S-Z The average WMAP observed and predicted radial profile for the 31 clusters. The continuum of the prediction curve is fixed by alignment with the 2o-3o data, which is at a level higher than that of the central 1o data points by 9σ (Q), 4.2σ (V), and 2.3σ (W).

  13. thus ....

  14. Axion  «Άξιον Εστί»

  15. Department of Physics, University of Patras* / Greece 18-20 May 2006 For Registration and Contribution, please contact: K. Zioutas zioutas@physics.upatras.gr Tel +41 76 4874592 Agenda TBA *Patras European Capital of Cultures 2006 Photo: The longest Bridge over sea in Europe in front of the University of Patras 2nd Joint ILIAS-CAST-CERN axion Training Workshop 2006 Speakers:F. Avignone (U. S.Carolina), K. Baker (Hampton U. & J.Lab), G. Cantatore (U. & INFN/Trieste), M. Davenport (CERN), E. Dudas (Paris & CERN), P. Geltenbort (ILL/Grenoble), I. Giomataris (Saclay), J. Huovelin (U. Helsinki), D. Hutsemekers (U. Liège), E. Masso (U. Barcelona), D. Miller (U. Chicago), P. Pugnat (CERN), A. Ringwald (DESY), C. Rizzo (UPS/CNRS Toulouse), Y. Semertzidis (BNL), P. Sikivie (U. Florida & CERN), R. Soufli (LLNL), E. Tziaferi (U. Sheffield), J. Vigen (CERN), Julia Vogel (U. Freiburg), I. Vergados (U. Ioannina) [TBC], K. Zioutas (U. Patras), K. Zurek (U. Washington assoc.)

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