K. Atapin, S. Fabrika

Transcription

1 K. Atapin, S. Fabrika Strasbourg

2 System SS433 The only known permanent superaccretor in the Galaxy Distance 5.5 kpc M~10 M Ṁ~10-4 M /year ~300Ṁ Edd v jet =0.26c L bol ~10 40 erg/s Wind funnel Jet Subcritical part of the disk 2

3 Supercritical disk was described by Shakura & Sunyaev (1973), Lipunova (1999), Poutanen et al. (2007) jet L=L edd (1+ln ṁ ) Spherization radius: R sp ~ R in ṁ ~ 10 9 cm Photosphere radius: R ph ~ cm Below R sp - supercritical part of the disk Above R sp - standard part of the disk Strong matter outflow, 99% of matter escapes the system 3

4 The system geometry P pr =162.15d P orb =13.08d i = ±0.05 θ = ±0.08 ϑ wf wf ψ=0 the most open funnel ψ=0.34, 0.66 closed (disk edge-on) Inclination angle 60 We never see the inner parts of the disc. They are always hidden by wind. 4

5 The system geometry If SS 433 were observed face-on, it would be the brightest X-ray source in the Milky Way. ULX (or ULS) ULX SS433 L x ~ эрг/с L opt ~10 39 эрг/с L jet ~ эрг/с L bol ~10 40 эрг/с 5

6 Power, Hz RXTE/PCA Power spectra β1=-0.06 Funnel is open Disk edge-on β2=-1.67 P f -α 1.34 α=-1.34 Frequency, Hz 6

7 ASCA Power spectra Funnel is open f l ~ Hz f h ~ Hz f h /f l ~ 180 7

8 Power Power States of Galactic black hole binaries high/soft low/hard Flat-toped noise is observed in low/hard (power-law) state, low accretion rate Frequency Frequency Pure power-law PDS is observed in high/soft (thermal dominant) state, high accretion rate (Belloni 2011, Ast. Nach., 332, 324) 8

9 Power, Power Power States of Galactic black hole binaries Disk edge-on high/soft Funnel is open low/hard This is not the case for SS433! Frequency Frequency Classical states of BHB is unusual for SS433 The shape of power spectrum tracks the 162-day precession period Funnel is open Disk edge-on The variability properties of SS433 is fully determined by wind funnel visibility SS433 This similarity of power spectra is only apparent (Belloni 2011, Ast. Nach., 332, 324) 9

10 List of analyzed ULXs (XMM-Newton data) Object NGC 5408 X-1 NGC 6946 X-1 M82 X-1 Holmberg II X-1 Holmberg IX X-1 NGC 1313 X-1 NGC 1313 X-2 NGC 4559 X-7 NGC 4559 X-10 NGC 5204 X-1 IC342 X-1 M81 X-6 Type SUL SUL SUL SUL HUL HUL BD SUL BD/HUL SUL HUL BD/HUL 10

11 Power spectrum of NGC5408 X-1 f l ~ Hz f h ~ Hz f QPO ~ Hz f h /f l ~ 50 f qpo /f h ~

12 Power spectrum of NGC6946 X-1 f l ~ Hz f h ~ Hz f QPO ~ Hz f h /f l ~ 100 f qpo /f h ~ 1.8

13 Power spectrum of M82 X-1 f QPO ~ 0.1 Hz 13

14 Other objects: there is no flat part NGC5204 X-1 soft NGC1313 X-1 hard Level of Poisson noise restricts detection of flat parts 14

15 Other objects: there is no flat part HoII X-1 soft HoIX X-1 hard Another type of variability 15

16 Результаты IC342 X-1 hard NGC4559 X-7 soft M81 X-6 hard NGC4559 X-10 hard 16

17 Other objects NGC1313 X-2 hard Source have shown very strong variability 17

18 Power Power Conclusions from observations NGC5408 X-1 NGC6946 X-1 M82 X-1 Other Frequency Frequency 18

19 Level of flat part / QPO level IC342 X-1 soft hard (Agrawal & Nandi 2015) Holmberg IX X-1 M82 X-1 (Dewangan et al. 2006, 641, 125) 19

20 Type C QPO Type C QPO is always associated with flat-topped noise Type C QPO frequency scales with BH mass Source f QPO, Hz M BHB ~10 NGC5408 X ~1000 (Dheeraj & Strohmayer 2012) HSS SIMS HIMS Type C (Belloni 2011, Ast. Nach., 332, 324) 20

21 Variability of supercritical disc Wind clumps intersect line of sight and "eclipse" innermost parts of the accretion disk which radiates in X-rays. (Middleton et al. 2011)

22 Variability of supercritical disc Why do QPO (and break) frequencies differ? 1)Different inclination 2)Different accretion rate (or both) Wind clumps intersect line of sight and "eclipse" innermost parts of the accretion disk which radiates in X-rays. (Middleton et al. 2011)

23 Power Variability of supercritical disc Why do QPO (and break) frequencies differ? 1)Different inclination 2)Different accretion rate other NCG1313 X-1 IC342 X-1 HoIX X-1 M82 X-1 NGC5408 X-1 NGC6946 X-1 SS433 SS433 NGC5408 X-1 NGC6946 X-1 NCG1313 X-1 IC342 X-1 HoIX X-1 other Frequency 23

24 Variability of supercritical disc Why do QPO (and break) frequencies differ? 1)Different inclination 2)Different accretion rate t cr r r sp 3/ 2 sp / ves rsp 5 m 3 f h m blob crossing time scale 3/ 2 break frequency Source f l, Hz f h, Гц Log(f h /f l ) Ṁ/Ṁ Edd SS NGC5408 X ~160 NGC6946 X ~50 SS433 NGC5408 X-1 NGC6946 X-1 24

25 Summary Only three of twelve analyzed sources shown flat parts in their power spectra. The flat parts of these ULXs are associated with QPO, however SS433 power spectrum haven t QPO. Other sources show about the same variability regardless of spectral type. The lower QPO/break frequency, the variability stronger. Shifting of frequencies may be caused by system inclination or difference of mass accretion rate. 25

26 Thank you 26