1 / 13

Intraday Variability and Images of Microquasar Cygnus X-3 †

Intraday Variability and Images of Microquasar Cygnus X-3 †. Jeong-Sook Kim 1,2 & Soon-Wook Kim 1 Astrophysics Research Group, KASI Kyunghee University

moesha
Download Presentation

Intraday Variability and Images of Microquasar Cygnus X-3 †

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript


  1. Intraday Variability and Images of Microquasar Cygnus X-3† • Jeong-Sook Kim1,2 & Soon-Wook Kim1 • Astrophysics Research Group, KASI • Kyunghee University • †Collaboration with Kurayama, Tomoharu (KVN/KASI) Honma, Mareki(VERA觀測所 /NAOJ) & Sasao, Tetsuo (前 KVN/KASI & VERA/NAOJ)

  2. Microquasars: introduction • Microquasars: Jet-ejecting X-ray binaires • Basic components of a microquasar are a spinning BH/NS, an accretion disk around it, and a collimated relativistic (or superluminal) jets, together with normal companion star. • Over fifty BH/NS transients are known • Most of jets have been usually observed with flares, presumably associated with instabilities in accretion disk.

  3. Cyg X-3:Restless,Frequently Flaring Microquasar (Jet-emitting XRB) • Difficulty for catching the radio jets (“microquasar phenomena”) in BH/NS X-ray binaries is due to their unpredictable, transient nature with the recurrence time-scale of a few to hundred years, while they are undetectable in quiescence. X-rays GRS 1915+105 Cygnus X-3 radio 500 days • Two radio-bright, frequently flaring microquasars: GRS 1915+105 & Cyg X-3. • Numerous VLBI/array studies for GRS 1915+105. 200 days • Cyg X-3, the radio-brightest, has been poorly studied (only 2 VLBI for small flares & 3 for giant flares) before our VERA observations, in spite of long-term monitoring for two decades ⇒ motivation • Goal: catching Variability (Flares) & Imaging (Jets) to study related physics of accretion and radiation processes.

  4. List of accepted proposal of VERA for Cygnus X-3

  5. VERA: Japanese VLBI Facility- VLBI Exploration of Radio Astrometry (Japan) Mizusawa 20m (& 10m) Correlation Center at Mitaka/NAOJ Mizusawa Ulsan Seoul KVN Jeju Iriki VERA Ogasawara 20m Ogasawara Iriki 20m Ishigaki Ishigaji-jima 20m

  6. Examples of VERA observation for Cyg X-3 • Time variability • Imaging

  7. Time variability:one baseline detection NRO45m-NiCT34m, 2004 • Top figure: ~30 min. flux variability in relatively low flux state with NRO45m-NiCT34m baseline in 2004. • Lower figure: recent observation at the MIZ-IRI baseline. • Variability time scale is apparently close to an hour in the flares with a peak of ~350 mJy. , 2008

  8. January May RXTE and RATAN monitoring in 2007 • Upper panel is the X-ray monitoring with RXTE all sky monitor in space. • We carried out VERA observation in January on the rise phase before the peak of a small, precursor flare, prior to the giant flare of 5.5 Jy. Light curve with red color is monitoring data of RATAN. • Unlike the case of January observation, no other radio observation so far has been reported before our May observation; hard to tell what was going on.

  9. ISH-MIZ Long baseline ISH-OGA MIZ-OGA MIZ-IRI IRI-OGA IRI-ISH Short baseline Imaging in 2007 2007 January • Cyg X-3 flared up to ~ 1Jy; plausibly at least 2 or 3 flares, although flux variation is different in each baseline. • Structure due to jets is plausible.

  10. ISH-MIZ ISH-OGA MIZ-OGA MIZ-IRI IRI-OGA IRI-ISH 2007 May • In the later half of our observation, Cyg X-3 flared up to ~ a few hundred mJy, lasting 2-3 hours, consistent for all baselines. • Possible flaring activity in the earlier epochs. • Jet-like structure is more evident than that in 2007 January. Baseline: Long-> short

  11. Summary of VERA Observations for Cyg X-3 • Time variabilities of ~30 min. & ~ hour were detected for low (tens of mJy) and higher (a few hundred mJy) flux states, consistent with other observations of Cyg X-3 and GRS 1915+105. • Plausible jet-like features for small flares peaked at ~ Jy could be obtained with VERA. However, for more detailed structure associated with jet activity, VERA-only observation with 6 baselines is not enough; collaboration with the East Asia VLBI facilities is required. The shorter baseline than VERA’s is necessary to study a detailed jet structure. • Radio monitoring like RATAN is important to describe what was going on before and after a detailed VBLI observation.

  12. Future Plan • Observations in 2007 & 2008 are under analysis. • Multi-wavelength study together with our VERA results is under investigation, focusing on the physics of accretion and radiation processes, and proper motion. • We will carry out 8 observations of Cyg X-3 for the 2008-2009 VERA open user observation.

  13. Thank you

More Related