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GAMMA-RAY COMPACT BINARIES* ASTROPHYSICAL SCENARIOS

GAMMA-RAY COMPACT BINARIES* ASTROPHYSICAL SCENARIOS. Félix Mirabel. * Neutron stars & Black holes in stellar binary systems that radiate in gamma-rays. (Will not refer to other types gamma-ray stellar binaries , e.g . Eta Carina) .

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GAMMA-RAY COMPACT BINARIES* ASTROPHYSICAL SCENARIOS

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  1. GAMMA-RAY COMPACT BINARIES*ASTROPHYSICAL SCENARIOS Félix Mirabel *Neutron stars & Black holes in stellarbinarysystemsthatradiate in gamma-rays. (Will not refer to other types gamma-ray stellarbinaries, e.g. Eta Carina)

  2. COMPACT GAMMA-RAY BINARIES IN 2006 The onlyknownwerePSR B1259-63, LSI +61 303 & LS 5039 Mirabel: Perspective in Science (2006) PSR B1259-63 • g-raysproduced by inverse Compton scattering: relativistic electrons collide with stellar and/or synchrotron photons and boost their energies to HE & VHE ranges. • In PSR B1259-63 the electrons are powered by the rotational energy of the pulsar. In microquasarsrelativistic electrons would come from accretion-powered jetsand in that publication I proposed as candidate sources Cyg X-1 & Cyg X-3.

  3. COMPACT GAMMA-RAY BINARIES IN 2012 Mirabel: Perspective in Science (2012) Sp Types of donors: Casares et al. (2012) HE, E>100 MeV & VHE, E>100 GeV PRODUCED BY LEPTONIC AND HADRONIC INTERACTIONS HE in superiorconjunction • Nameg-ray s Sp Type • PSR B1259-63 HE, VHE O9.5 Ve • AGL J2241+4454 HE ? B3 IV ne+sh • HESS J0631+057 VHE B0 Vpe • LS I+61 303HE, VHE B0 Ve(?) • Nameg-rays Sp Type • Cyg X-3 HE WNE([2,5]) • Cyg X-1 HE, VHE? O7 V • LS I+61 303 HE, VHE B0 Ve (?) Nameg-ray s Sp Type LS 5039 HE, VHE O6.5 V((f)) 1FGL J1018 HE, VHE? O6 V((f)) • g-raybinaries are NSs and BHsorbiting massive stars • So far no detection of any LMXB (e.g. GRS 1915+105) • The g-rayemissionismodulatedwith the orbital periodand/or periastron

  4. In thiscontext, high photon stadistics at a few tensof GeVswouldbe an advantageto unambiguously identify compact gamma-ray binaries in the Milky Way, In this area of research, (namely “Compact g–ray binaries”), it would be convenient if CTA could have a low energy threshold. This is also the case to make progress in other areas of high energy astrophysics, such as in studies of Pulsars, GRBs, AGN…

  5. FUTURE CHALLENGES IN THIS AREA OF RESEARCH • The typical confusion in star formation regionscanbeovercomed by correlatedmulti-l orbital modulations in the gamma-rays, X-rays, IR, and radio waves. (e.g. Cyg X-3, 1FGL J1018.6-5856). • CTA mayprovide the required photon statistics for highsensitivity and angularresolution, thatwouldidentify a larger population of compact gamma-ray sources in the MilkyWay. • Since as compact binaries, AGN, blazars, GRBs & neutron stars are rapidly variable sources of g-rays, the “CTA-STAC underlines the importance of all the detector systems, SST, MST andLST, for making possible observations with unique sensitivity, includingtransient sources down to 20 GeV »

  6. OLD SIMULATION AS A FUNCTION OF ALTITUDE

  7. NEW SIMULATION UP TO 50 GeV AS A FUNCTION OF ALTITUDE FOR 50h Maier (2013) presented by Hinton at the CTA SSC 2000 m 3700 m • Wouldthe sensitivitychange for muchshorterexposures? • Could the simulationsbeextended down to 20 Gev?

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