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Unraveling Cosmic Mysteries: Insights from High-Energy Astrophysics Observations

This research delves into the intriguing behaviors of black hole transients, neutron star activities, and supernovae, approached through advanced observational techniques including Suzaku, Swift, and MAXI. With a focus on correlations between X-ray emissions and cosmic-ray acceleration, we analyze key phenomena such as Seyfert 2 galaxies and blazars, emphasizing the importance of multi-observatory collaboration. Our findings on time-domain variability and state transitions add significant knowledge to the astrophysical landscape, shedding light on dark energy and galaxy formation dynamics.

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Unraveling Cosmic Mysteries: Insights from High-Energy Astrophysics Observations

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  1. Scientific research ? Getting results from limited information.

  2. Astrophysical view Seyfert2! Dark Energy?? . Universe Blazar? Galaxy formation .. Cosmic-ray Acceleration ….

  3. Time domain 104 + BH trasients + NS transient + Super Nova + Classical Nova + Flaring stars + AGN long term variability 102 1 Variability (day) 10–2 Pulsars GRBs / SRFs 10–4 103 10–3 1 10–9 10–6 ~ 5yr Observational duration (day)

  4. Black hole candidatesNew Activity, Spectral Transition ATEL#2711 Soft X-ray increase ATEL#2380 Beginning of new activity ATEL#2404, #2635 State transition Cyg X-1 GX 339-4 Cyg X-3 2-4 keV 4-10 keV 10-20keV ~ 1yr O-07: Negoro, YO-04amaoka, P-01 Nakahira, P-07Shidatsu

  5. Suzaku observation of XTE J1752-223 Suzaku observation Details of observations • ObservationDate2010-02-24 04:58:00 – 2010-02-25 04:27:24 (UT) • Total exposure 41 ksec • ＸＩＳ Exposure0.5 ksec (XIS 1), 6.1 ksec (XIS 0,3) • Observation directionHXD nominal • ＸＩＳ mode • Full window 0.1s burst option (XIS 1) 1/4 window 0.3s burst option (XIS 0.3) Suzaku observed “High/Soft state” Low/hard High/Soft

  6. MAXI J1409-619 confirmed and accurately localized by Swift • MAXI detection of outbursts X-ray count rate Date Swift XRT Oct. 21 O-07 Kennea

  7. Time domain 104 We have expected and already learned: + BH trasients + NS transient + Super Nova + Classical Nova + Flaring stars + AGN long term variability Collaboration & Coordinate observation With other observatories Is crucially important!! 102 1 Variability (day) 10–2 Pulsars GRBs / SRFs 10–4 103 10–3 1 10–9 10–6 ~ 5yr Observational duration (day)

  8. Time domain 104 We have already learned: + BH trasients + NS transient + Super Nova + Classical Nova + Flaring stars + AGN long term variability Collaboration & Coordinate observation With other observatories Is crucially important!! 102 Swift Fermi INTEGRAL 1 Variability (day) CRTS PTF LSST 10–2 Pulsars GRBs / SRFs 10–4 103 10–3 1 10–9 10–6 ~ 5yr Observational duration (day)

  9. MAXI project started more than 1.5 decades ago!2nd MAXI Workshop in 2001

  10. We got old …. Mihara

  11. Prof Matsuoka was young …. Many thanks to Prof. Matsuoka for his hard work and elaborations !!!

  12. This workshop partially supported by Aoyama Gakuin University Research Institute and Society for Promotion of Space Science. We thank to Dr. Kohama, Ms. Takahashi, Mr. Adachi, and Ms. Konagai. The organizers would thank to all the participants for coming.

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