Giant Flares and Offstates
|
|
|
- Naomi Sanders
- 5 years ago
- Views:
Transcription
1 Highly structured Wind in Vela X-1: Giant Flares and Offstates Ingo Kreykenbohm (Dr. Karl-Remeis-Sternwarte, Bamberg) J. Wilms, P. Kretschmar, J.Torrejon, K. Pottschmidt, M. Hanke, A. Santangelo, C. Ferrigno, R. Staubert ESAC Science Seminar, November 20, 2008 ESA
2 X-ray Binaries accretion most efficient energy source! 1 accreted electron: 100keV accretion rate: g/sec UCSD 2
3 X-ray Binaries accretion most efficient energy source! 1 accreted electron: 100keV accretion rate: g/sec compact object + optical star UCSD 2
4 X-ray Binaries accretion most efficient energy source! 1 accreted electron: 100keV accretion rate: g/sec compact object + optical star classification LMXBs UCSD 2
5 X-ray Binaries accretion most efficient energy source! 1 accreted electron: 100keV accretion rate: g/sec compact object + optical star classification LMXBs Roche Lobe Overflow - accretion disk - old system - weak magnetic field - no pulsations UCSD 2
6 X-ray Binaries NASA 3
7 X-ray Binaries compact object + optical star NASA 3
8 X-ray Binaries compact object + optical star classification HMXB NASA 3
9 X-ray Binaries compact object + optical star classification HMXB Wind accretion Be mechanism NASA 3
10 X-ray Binaries compact object + optical star classification HMXB Wind accretion Be mechanism - young systems - strong magnetic field - pulsations NASA 3
11 X-ray Pulsars 4
12 X-ray Pulsars Neutron stars have strong magnetic field: B~10 12 G (flux conservation in SN collaps) 4
13 X-ray Pulsars Neutron stars have strong magnetic field: B~10 12 G (flux conservation in SN collaps) material couples to magnetic field lines material is channeled onto the magnetic poles hotspots emerge 4
14 X-ray Pulsars Neutron stars have strong magnetic field: B~10 12 G (flux conservation in SN collaps) material couples to magnetic field lines material is channeled onto the magnetic poles hotspots emerge offset of magnetic and rotational axis pulsations 4
15 Cyclotron Lines strong magnetic field: electron energies are quantized in Landau levels: B e 5
16 Cyclotron Lines strong magnetic field: electron energies are quantized in Landau levels: E cyc = he = 11.6 kev m e c2 ( B ) G 12-B-12 B e 5
17 Cyclotron Lines strong magnetic field: electron energies are quantized in Landau levels: E cyc = he = 11.6 kev m e c2 ( B ) G Cyclotron resonance scattering 12-B-12 B features (CRSFs) e 5
18 Cyclotron Lines strong magnetic field: electron energies are quantized in Landau levels: E cyc = he = 11.6 kev m e c2 ( B ) G Cyclotron resonance scattering 12-B-12 B features (CRSFs) e E n = ne cyc = (1 + z)e n,obs 5
19 Cyclotron Lines strong magnetic field: electron energies are quantized in Landau levels: E cyc = he = 11.6 kev m e c2 ( B ) G 12-B-12 Cyclotron resonance scattering features (CRSFs) E n = ne cyc = (1 + z)e n,obs First obsrvation by Truemper et al. in 1977 in Hercules X-1: 5
20 Cyclotron Lines strong magnetic field: electron energies are quantized in Landau levels: E cyc = he = 11.6 kev m e c2 ( B ) G 12-B-12 Emission Cyclotron resonance scattering features (CRSFs) E n = ne cyc = (1 + z)e n,obs First obsrvation by Truemper et al. in 1977 in Hercules X-1: 5
21 Cyclotron Lines strong magnetic field: electron energies are quantized in Landau levels: E cyc = he = 11.6 kev m e c2 ( B ) G 12-B-12 Emission Cyclotron resonance scattering features (CRSFs) E n = ne cyc = (1 + z)e n,obs First obsrvation by Truemper et al. in 1977 in Hercules X-1: Ecyc = 40 kev Absorption 5
22 Vela X-1 HD NS + B0.5Ib GP Vel super giant companion photoionization wake dense Wind: tidal stream Vela X-1 Ṁ = M accretion wake Strömgren sphere orbital Period 8.96 d heaviest known neutron star: 1.8 M ESA6
23 Vela X a) Vela X!1 (RXTE) NS + B0.5Ib GP Vel super giant companion dense Wind: Ṁ = M o a ed cou ts/sec/ ev orbital Period 8.96 d heaviest known neutron star: 1.8 M!! 5 0!5 5 0 b) c)!5 typical XRB spectrum CRSFs at 25 and 50keV! 5 0!5 d) 6
24 History Haberl (1994) Vela X-1 known to be variable: Flares: ROSAT, Granat, EXOSAT, RXTE 7
25 History Haberl & White (1990) Vela X-1 known to be variable: Flares: ROSAT, Granat, EXOSAT, RXTE 7
26 History Vela X-1 known to be variable: Flares: ROSAT, Granat, EXOSAT, RXTE 7
27 History Vela X-1 known to be variable: Inoue (1984) Flares: ROSAT, Granat, EXOSAT, RXTE Dips : Tenma, Granat, RXTE various ideas, cause unkown 8
28 History Vela X-1 known to be variable: Flares: ROSAT, Granat, EXOSAT, RXTE Dips : Tenma, Granat, RXTE various ideas, cause unkown 8
29 INTEGRAL a) Flare 1 Flare 2 Flare 4 Flare 5 Flare 3 Countrate (counts/s) Hardness Ratio 0!0.65!0.70!0.75!0.80!0.85 b) Rev 137 Rev 138 Rev 139 Rev 140 Rev November 2003 December 9
30 INTEGRAL Countrate (counts/s) a) Flare 1 Flare 2 Flare 4 Flare 5 Flare Crab Fluence: 1.2x10 41 Rev 137 Rev 138 Rev 139 Rev 140 Rev 141 Hardness Ratio!0.65!0.70!0.75!0.80!0.85 b) November 2003 December 9
31 INTEGRAL Countrate (counts/s) a) Flare 1 Flare 2 Flare 4 Flare 5 Flare 3 short flare Rev 137 Rev 138 Rev 139 Rev 140 Rev 141 Hardness Ratio!0.65!0.70!0.75!0.80!0.85 b) November 2003 December 9
32 INTEGRAL Countrate (counts/s) a) Flare 1 Flare 2 Flare 4 Flare 5 Flare 3 long flare Fluence: 1.2x10 41 Rev 137 Rev 138 Rev 139 Rev 140 Rev 141 Hardness Ratio!0.65!0.70!0.75!0.80!0.85 b) November 2003 December 9
33 Flares Flare 1: Peak: 5.2 Crab Duration: sec spectrum softer fast rise: τ = 0.15 Countrate (counts/s) Time [MJD!52971] November 28 τ = Trise / Ttotal 10
34 Flares Flare 1: Peak: 5.2 Crab Duration: sec spectrum softer fast rise: τ = 0.15 Flare 3: Peak 5.3 Crab Duration 1800 sec fast rise: τ = 0.28 (o*+tr.te!01o*+t2324 '""" &"" %"" $"" #"" " <i7e!>?@6!:#a;%b! "9:$ "9:: "9:% "9:; "9:& '5 '5C'" '5C#" '5C5" '5C$" '5C:" '$ #""5!6e1e78er!5 τ = Trise / Ttotal 10
35 Hardness a) Flare 1 Flare 2 Flare 4 Flare 5 Flare 3 Countrate (counts/s) Hardness Ratio 0!0.65!0.70!0.75!0.80!0.85 b) Rev 137 Rev 138 Rev 139 Rev 140 Rev November 2003 December 11
36 Hardness Countrate (counts/s) a) Flare 1 Flare 2 Flare 4 Flare 5 Flare 3 significant spectral change Rev 137 Rev 138 Rev 139 Rev 140 Rev 141 Hardness Ratio!0.65!0.70!0.75!0.80!0.85 b) November 2003 December 11
37 Hardness Countrate (counts/s) a) Flare 1 Flare 2 Flare 4 Flare 5 Flare 3 significant spectral change Rev 137 Rev 138 Rev 139 Rev 140 Rev 141 Hardness Ratio!0.65!0.70!0.75!0.80!0.85 b) November 2003 December 11
38 Hardness a) Flare 1 Flare 2 Flare 4 Flare 5 Flare 3 Countrate (counts/s) significant spectral change no change Hardness Ratio 0!0.65!0.70!0.75!0.80!0.85 b) Rev 137 Rev 138 Rev 139 Rev 140 Rev November 2003 December 11
39 HID Intensity (20!40 kev) Flare 1 Flare 2 Flare 4 Flare 5 0!0.9!0.8!0.7!0.6 Hardness Flare 1 Flare 2 Flare 3 Flare 4 Flare 5 τ=0.15 τ=0.83 τ=0.28 τ=0.13 τ=
40 HID hardness mostly constant (no evolution w/ phase) Intensity (20!40 kev) Flare 1 Flare 2 Flare 4 Flare 5 0!0.9!0.8!0.7!0.6 Hardness Flare 1 Flare 2 Flare 3 Flare 4 Flare 5 τ=0.15 τ=0.83 τ=0.28 τ=0.13 τ=
41 HID hardness mostly constant (no evolution w/ phase) significant change during Flares 1 and 4 NO change during Flares 2 and 5 Intensity (20!40 kev) Flare 1 Flare 2 Flare 4 Flare 5 0!0.9!0.8!0.7!0.6 Hardness Flare 1 Flare 2 Flare 3 Flare 4 Flare 5 τ=0.15 τ=0.83 τ=0.28 τ=0.13 τ=
42 HID hardness mostly constant (no evolution w/ phase) significant change during Flares 1 and 4 NO change during Flares 2 and 5 two types of flares: fast rise, spectral change slow rise, no spectral change Intensity (20!40 kev) Flare 1 Flare 2 Flare 4 Flare 5 0!0.9!0.8!0.7!0.6 Hardness Flare 1 Flare 2 Flare 3 Flare 4 Flare 5 τ=0.15 τ=0.83 τ=0.28 τ=0.13 τ=
43 Offstates a) Flare 1 Flare 2 Flare 4 Flare 5 Flare 3 Countrate (counts/s) Hardness Ratio 0!0.65!0.70!0.75!0.80!0.85 b) Rev 137 Rev 138 Rev 139 Rev 140 Rev November 2003 December 14
44 Offstates a) Flare 1 Flare 2 Flare 4 Flare 5 Flare 3 Countrate (counts/s) Hardness Ratio 0!0.65!0.70!0.75!0.80!0.85 b) Rev 137 Rev 138 Rev 139 Rev 140 Rev November 2003 December 14
45 Offstates 120 Time [MJD!52980] Countrate (counts/s) December 8 15
46 Offstates quasi periodic behavior Period: 6820 sec 120 Time [MJD!52980] Countrate (counts/s) December 8 15
47 Offstates quasi periodic behavior Period: 6820 sec 120 Time [MJD!52980] flux decreases to zero Countrate (counts/s) December 8 15
48 Offstates 5 offstates detected extremely rapidly 0 to ~100 cts/sec similar to previous no residual flux detectable countrate drops / increases increase within 20 sec from duration sec offstates, but observed in detail Countrate (counts/s) Time [MJD!52981] :10 8:20 8:30 8:40 8:50 9: December
49 Discussion wind in a HMXB system very complex (X-ray photoionization...) time dependence (CAK wind model not sufficient) need 2D/3D simulations short flares: highly variable density/velocity structure shock fronts, dense filaments, accretion stream oscillates: flip-flop instability Taam & Fryxell (1989) predicted time scales: flares ~45min (flares 2,3,4)! 17
50 Discussion wind in a HMXB system very complex (X-ray photoionization...) time dependence (CAK wind model not sufficient) need 2D/3D simulations short flares: highly variable density/velocity structure shock fronts, dense filaments, accretion stream oscillates: flip-flop instability Blondin et al. (1990) predicted time scales: flares ~45min (flares 2,3,4)! 17
51 Discussion 18
52 Discussion no structured wind necessary so far: presence of NS causes structure 18
53 Discussion log density (g/cm 3 ) no structured wind necessary so far: presence of NS causes structure 5x10 10 cm 18
54 Discussion log density (g/cm 3 ) no structured wind necessary so far: presence of NS causes structure BUT: long flares 1 & 5: can not be explained by flip-flop instability blobs (or clumps) in the stellar wind But: flares quite long and Blobs very fast! significant fraction of binary orbit 5x10 10 cm blob is viscously smeared out in accretion disk 18
55 Discussion log density (g/cm 3 ) no structured wind necessary so far: presence of NS causes structure BUT: long flares 1 & 5: can not be explained by flip-flop instability blobs (or clumps) in the stellar wind But: flares quite long and Blobs very fast! significant fraction of binary orbit 5x10 10 cm blob is viscously smeared out in accretion disk can feed NS for several hours (flares 1 & 5) 18
56 Discussion Offstates: absorption impossible not only blobs but also holes in stellar wind! density drops by factor 10 5 Runacres & Owocki (2005) 19
57 SFXTs drop in acc. rate why no pulsations? why so sudden? onset of propeller effect? calculate flux for onset of propeller: F X = ( B ) 2 P 7/3 ( d 1kpc ) 2 ( M 1.4M ) 2/3 FX = 1.1 x erg cm -2 s erg s -1 very close to what is observed for Vela X-1! 20
58 SFXTs drop in acc. rate why no pulsations? why so sudden? onset of propeller effect? calculate flux for onset of propeller: F X = ( B ) 2 P 7/3 ( d 1kpc ) 2 ( M 1.4M ) 2/3 FX = 1.1 x erg cm -2 s erg s -1 very close to what is observed for Vela X-1! Vela X-1 enters region of low density propeller 20
59 SFXTs 21
60 SFXTs SFXTs (Supergiant Fast X-ray Transients) mostly below detection limit at > 20keV exhibit very short flares 21
61 SFXTs SFXTs (Supergiant Fast X-ray Transients) mostly below detection limit at > 20keV exhibit very short flares hardness ratio changes sometimes over flare 21
62 SFXTs SFXTs (Supergiant Fast X-ray Transients) mostly below detection limit at > 20keV exhibit very short flares hardness ratio changes sometimes over flare Grebenev & Sunyaev (2007): SFXTs bright objects, but mostly in propeller regime 21
63 SFXTs SFXTs (Supergiant Fast X-ray Transients) mostly below detection limit at > 20keV exhibit very short flares hardness ratio changes sometimes over flare Grebenev & Sunyaev (2007): SFXTs bright objects, but mostly in propeller regime Vela X-1 just opposite: rarely in propeller regime 21
64 Conclusions stellar wind in Vela X-1 is structured (clumps, holes) short and long flares up to 5.3 Crab Hardness ratio changes during rapidly rising flares also (sometimes) seen in SFXTs Offstates with no flux detected by ISGRI can be explained by triggering propeller effect 22
65 Conclusions stellar wind in Vela X-1 is structured (clumps, holes) short and long flares up to 5.3 Crab Hardness ratio changes during rapidly rising flares also (sometimes) seen in SFXTs Offstates with no flux detected by ISGRI can be explained by triggering propeller effect Vela X-1 is quite similar to SFXTs 22
66 Conclusions stellar wind in Vela X-1 is structured (clumps, holes) short and long flares up to 5.3 Crab Hardness ratio changes during rapidly rising flares also (sometimes) seen in SFXTs Offstates with no flux detected by ISGRI can be explained by triggering propeller effect Vela X-1 is quite similar to SFXTs Thank you for your attention! 22
PoS(Integral08)120. Scanning the Egress of Vela X-1
P. Kretschmar a, I. Kreykenbohm b, J. Wilms b, M. Hanke b, M. Stuhlinger a, A.M.T. Pollock a, R. Staubert c, E. Kendziorra c, R. Rothschild d and S. Suchy d E-mail: peter.kretschmar@esa.int a ESA European
Monte Carlo simulation of cyclotron resonant scattering features
of cyclotron resonant scattering features Dr. Karl Remeis-Sternwarte Bamberg, Sternwartstraße 7, 96049 Bamberg, Germany Erlangen Centre for Astroparticle Physics (ECAP), Erwin-Rommel-Str. 1, 91058 Erlangen,
Distribution of X-ray binary stars in the Galaxy (RXTE) High-Energy Astrophysics Lecture 8: Accretion and jets in binary stars
High-Energy Astrophysics Lecture 8: Accretion and jets in binary stars Distribution of X-ray binary stars in the Galaxy (RXTE) Robert Laing Primary Compact accreting binary systems Compact star WD NS BH
Isolated And Accreting Magnetars Viewed In Hard X-rays
The XXVII Texas Symposium on Relativistic Astrophysics Isolated And Accreting Magnetars Viewed In Hard X-rays Wei Wang National Astronomical Observatories, Beijing China Dec 8 13 2013, Dallas TX, USA Contents
Probing the stellar wind environment of Vela X-1. With MAXI: hints for a multi-tasking accretion wake
Probing the stellar wind environment of Vela X-1 With MAXI: hints for a multi-tasking accretion wake Christian Malacaria (IAAT + RIKEN) Mihara T., Makishima K., Matsuoka M., Morii M., Sugizaki M. (RIKEN),
4U : a well-hidden pearl
Dr. Karl-Remeis Sternwarte Bamberg Astronomical Institute of the Friedrich-Alexander-University Erlangen-Nuremberg Erlangen Centre for Astroparticle Physics (ECAP) Ingo Kreykenbohm, Laura Barragán, Jörn
arxiv: v1 [astro-ph] 16 Oct 2008
![arxiv: v1 [astro-ph] 16 Oct 2008](/thumbs/88/114778887.jpg "arxiv: v1 [astro-ph] 16 Oct 2008")
Astronomy & Astrophysics manuscript no. 9956 c ESO 2018 September 28, 2018 High variability in Vela X-1: giant flares and off states Ingo Kreykenbohm 1,2,3,4, Jörn Wilms 1,2, Peter Kretschmar 5, José Miguel
The Be/X-ray binary V
The Be/X-ray binary V 0332+53 C. Ferrigno, V. Savchenko, M. Kühnel, L. Ducci,. P. Kretschmar, K. Pottschmidt, J. Wilms, E. Bozzo, C. Malacaria, A. Santangelo, G. Schönherr 1 Introduction High mass X-ray
arxiv: v1 [astro-ph.he] 29 Jan 2014
![arxiv: v1 [astro-ph.he] 29 Jan 2014](/thumbs/77/74657220.jpg "arxiv: v1 [astro-ph.he] 29 Jan 2014")
Mon. Not. R. Astron. Soc., () Printed 4 February 8 (MN LATEX style file v.) Variations and Correlations in Cyclotron Resonant Scattering Features of Vela X- Studied by INTEGRAL arxiv:4.74v [astro-ph.he]
Cyclotron lines in accreting X-ray pulsars. - models and observations -
Cyclotron lines in accreting X-ray pulsars - models and observations - Gabriele Schönherr - AIP, Germany on behalf of the MAGNET collaboration: J. Wilms (FAU, Germany), P. Kretschmar (ESAC,Spain), I. Kreykenbohm
Deciphering the accretion structure in Vela X-1
Deciphering the accretion structure in Vela X-1 Victoria Grinberg MIT Kavli Institute for Astrophysics and Space Research N. Hell, M.A. Nowak, D. Huenemoerder, N.S. Schulz, M. Kühnel, J. Wilms, F. Fürst,
A propelling neutron star in the enigmatic Be-star γ Cassiopeia
A propelling neutron star in the enigmatic Be-star γ Cassiopeia Konstantin Postnov (Moscow University, Sternberg Astronomical Institute) Physics of Neutron Stars 2017 St. Petersbourg, July 14, 2017 PK,
Accreting Binary Pulsars
Accreting Binary Pulsars A test bed for matter under extreme conditions Mauro Orlandini INAF/IASF Bologna CSV Rev: 0.2 (2015/09/09) Ferrara PhD School Accreting Systems / Spectral Ferrara, 09/09/2015 Portrait
Variations and correlations in cyclotron resonant scattering features of
Advance Access publication 2014 March 19 doi:10.1093/mnras/stu210 Variations and correlations in cyclotron resonant scattering features of Vela X-1 studied by INTEGRAL Wei Wang National Astronomical Observatories,
arxiv: v3 [astro-ph.he] 28 Nov 2011
![arxiv: v3 [astro-ph.he] 28 Nov 2011](/thumbs/93/112650562.jpg "arxiv: v3 [astro-ph.he] 28 Nov 2011")
arxiv:1105.1907v3 [astro-ph.he] 28 Nov 2011 1, Erik Kuulkers 2, Peter Kretschmar 2, Stefan Larsson 3, Konstantin Postnov 4, Al. Yu. Kochetkova 4, and Mark H. Finger 5,6 1 Department of Physics, Systems
High Mass X-ray Binaries hosting a neutron star: a review
High Mass X-ray Binaries hosting a neutron star: a review Lara Sidoli INAF-IASF Milano, Italy Congresso Nazionale Oggetti Compatti CNOC IX Osservatorio di Monte Porzio Catone 22-25 settembre 2015 1 High
Cyclotron Line Science with LAXPC. Dipankar Bhattacharya IUCAA, Pune
Cyclotron Line Science with LAXPC Dipankar Bhattacharya IUCAA, Pune Workshop on Science with LAXPC/Astrosat, Hyderabad, 16 December 2014 A High Mass X-ray Binary Cyclotron Resonant Scattering Features
arxiv: v1 [astro-ph.he] 20 Oct 2011
![arxiv: v1 [astro-ph.he] 20 Oct 2011](/thumbs/92/110986291.jpg "arxiv: v1 [astro-ph.he] 20 Oct 2011")
Bull. Astr. Soc. India (2) 39, 2 arxiv:.4446v [astro-ph.he] 2 Oct 2 Transient High Mass X-ray Binaries Biswajit Paul and Sachindra Naik 2 Raman Research Institute, Sadashivnagar, C. V. Raman Avenue, Bangalore
Accretion in Binaries
Accretion in Binaries Two paths for accretion Roche-lobe overflow Wind-fed accretion Classes of X-ray binaries Low-mass (BH and NS) High-mass (BH and NS) X-ray pulsars (NS) Be/X-ray binaries (NS) Roche
X-ray binaries. Marat Gilfanov MPA, Garching
X-ray binaries Marat Gilfanov MPA, Garching Outline observational appearance populations in galaxies relation to star-formation history numbers, luminosity distributions, IMF Hans-Jakob Grimm (CfA) Igor
Evolution of High Mass stars
Evolution of High Mass stars Neutron Stars A supernova explosion of a M > 8 M Sun star blows away its outer layers. The central core will collapse into a compact object of ~ a few M Sun. Pressure becomes
XMM-Newton's view of the multiple uorescence lines of GX 301 2
XMM-Newton's view of the multiple uorescence lines of GX 31 2 Felix Fürst Dr. Karl Remeis-Sternwarte Bamberg Erlangen Centre for Astroparticle Physics (ECAP) Friedrich-Alexander-University Erlangen-Nuremberg
X-ray observations of X-ray binaries and AGN
X-ray observations of X-ray binaries and AGN Tomaso M. Be!oni (INAF - Osservatorio Astronomico di Brera) (Visiting Professor, Univ. of Southampton) OUTLINE Lecture I: Accretion onto compact objects, X-ray
Formation and evolution of supergiant High Mass X-ray Binaries
Formation and evolution of supergiant High Mass X-ray Binaries, F. Fortin, W. Massonneau CEA, Université Paris Diderot Institut Universitaire de France The Impact of Binaries on Stellar Evolution ESO Worshop,
FORMATION AND EVOLUTION OF COMPACT BINARY SYSTEMS
FORMATION AND EVOLUTION OF COMPACT BINARY SYSTEMS Main Categories of Compact Systems Formation of Compact Objects Mass and Angular Momentum Loss Evolutionary Links to Classes of Binary Systems Future Work
Unstable Mass Transfer
Unstable Mass Transfer When the mass ratios are large, or when the donor star has a deep convective layer (so R M-1/3), mass loss will occur on a dynamical timescale. The result will be common envelope
The BAT Hard X-ray Monitor and Survey: 10+ years running. Hans A. Krimm NASA Goddard Space Flight Center Greenbelt, MD USA USRA / CRESST
The BAT Hard X-ray Monitor and Survey: 10+ years running Hans A. Krimm NASA Goddard Space Flight Center Greenbelt, MD USA USRA / CRESST Swift/BAT overview 14-195 kev energy range FOV: 1.94 sr (> 10% coding)
Cyclotron Observations of Binary X-Ray Pulsars
Progress of Theoretical Physics Supplement No. 169, 2007 191 Cyclotron Observations of Binary X-Ray Pulsars Tatehiro Mihara, 1, ) Yukikatsu Terada, 1 Motoki Nakajima, 2 Motoko Suzuki, 1 Teruaki Enoto,
Orbital evolution and apsidal motion studies: Transient sources. 3.1 Introduction
53 CHAPTER 3. Orbital evolution and apsidal motion studies: Transient sources 3.1 Introduction In the previous chapter we described our study of persistent X-ray binary pulsars and their orbital evolution.
Pulsars ASTR2110 Sarazin. Crab Pulsar in X-rays
Pulsars ASTR2110 Sarazin Crab Pulsar in X-rays Test #2 Monday, November 13, 11-11:50 am Ruffner G006 (classroom) Bring pencils, paper, calculator You may not consult the text, your notes, or any other
The magnetic spectrum of X-ray binary pulsars
The magnetic spectrum of X-ray binary pulsars C. Ferrigno & R. Farinelli ISDC & ESSC, University of Geneva 1 High B-field: an ubiquitous property High mass X-ray binaries are normally young systems, where
Pulse phase resolved spectroscopy: Probe of the dip phenomenon in the pulse profiles of GX 304-1
Chapter 4 Pulse phase resolved spectroscopy: Probe of the dip phenomenon in the pulse profiles of GX 34-1 4.1 Introduction GX 34-1 (4U 158-61) is a transient high-mass X-ray binary pulsar discovered using
Millisecond X-ray pulsars: 10 years of progress. Maurizio Falanga
Millisecond X-ray pulsars: 10 years of progress Maurizio Falanga History I Radio Astronomy in the 30 s-60 s Karl Jansky 1933 3C273 Discovery (1961-63) Quasi-Stellar Radio Sources as the most energetic
arxiv: v1 [astro-ph.he] 24 Dec 2013
![arxiv: v1 [astro-ph.he] 24 Dec 2013](/thumbs/92/108440419.jpg "arxiv: v1 [astro-ph.he] 24 Dec 2013")
Research in Astron. & Astrophys. Vol. (x) No., (http://www.raa-journal.org) Research in Astronomy and Astrophysics arxiv:3.6753v [astro-ph.he] 4 Dec 3 Temporal Variations And Spectral Properties of Be/X-ray
Dr. Reed L. Riddle. Close binaries, stellar interactions and novae. Guest lecture Astronomy 20 November 2, 2004
Dr. Reed L. Riddle Close binaries, stellar interactions and novae Guest lecture Astronomy 20 November 2, 2004 Gravitational Tides Look at the forces acting on one body orbiting another - more pull on closer
arxiv: v1 [astro-ph.he] 10 Sep 2013
![arxiv: v1 [astro-ph.he] 10 Sep 2013](/thumbs/71/66202890.jpg "arxiv: v1 [astro-ph.he] 10 Sep 2013")
The Journal s name will be set by the publisher DOI: will be set by the publisher c Owned by the authors, published by EDP Sciences, 213 arxiv:139.252v1 [astro-ph.he] 1 Sep 213 On the origin of cyclotron
Gamma-ray binaries as pulsars spectral & variability behaviour Guillaume Dubus. Laboratoire d Astrophysique de Grenoble UMR 5571 UJF / CNRS
Gamma-ray binaries as pulsars spectral & variability behaviour Guillaume Dubus Laboratoire d Astrophysique de Grenoble UMR 5571 UJF / CNRS Image: Mirabel 2006 1 Pulsars & massive stars Young pulsars, magnetic
The Search for Cyclotron Resonant Scattering Harmonics in the Hard Spectra of Accreting Pulsars. Andrea Santangelo IASF-CNR Sez.
The Search for Cyclotron Resonant Scattering Harmonics in the Hard Spectra of Accreting Pulsars Andrea Santangelo IASF-CNR Sez. Palermo Contents Introduction Review of the Observational Results AXRBPs
Neutron Stars. Neutron Stars and Black Holes. The Crab Pulsar. Discovery of Pulsars. The Crab Pulsar. Light curves of the Crab Pulsar.
Chapter 11: Neutron Stars and Black Holes A supernova explosion of an M > 8 M sun star blows away its outer layers. Neutron Stars The central core will collapse into a compact object of ~ a few M sun.
arxiv: v2 [astro-ph.he] 18 Feb 2016
![arxiv: v2 [astro-ph.he] 18 Feb 2016](/thumbs/85/92999281.jpg "arxiv: v2 [astro-ph.he] 18 Feb 2016")
Astronomy& Astrophysics manuscript no. velamalacaria_revised c ESO 2018 April 2, 2018 Probing the stellar wind environment of Vela X-1 with MAXI C. Malacaria 1, 2, T. Mihara 2, A. Santangelo 1, K. Makishima
6 th lecture of Compact Object and Accretion, Master Programme at Leiden Observatory
6 th lecture of Compact Object and Accretion, Master Programme at Leiden Observatory Accretion 1st class study material: Chapter 1 & 4, accretion power in astrophysics these slides at http://home.strw.leidenuniv.nl/~emr/coa/
Chandra-HETGS Observations of LMC X-1. Michael Nowak, Ron Remillard, Norbert Schulz (MIT-Kavli) & Jörn Wilms (University of Bamberg)
Chandra-HETGS Observations of LMC X-1 Michael Nowak, Ron Remillard, Norbert Schulz (MIT-Kavli) & Jörn Wilms (University of Bamberg) One of the few persistent BHC HMXB: Focused Wind-Fed Soft X-ray Dominated
arxiv: v1 [astro-ph.he] 14 Feb 2013
![arxiv: v1 [astro-ph.he] 14 Feb 2013](/thumbs/84/90977748.jpg "arxiv: v1 [astro-ph.he] 14 Feb 2013")
arxiv:1302.3434v1 [astro-ph.he] 14 Feb 2013 European Space Astronomy Centre (ESA/ESAC), Science Operations Department, Villanueva de la Cañada (Madrid), Spain E-mail: peter.kretschmar@esa.int Elisa Nespoli
Cataclysmic variables
Cataclysmic variables Sander Bus Kapteyn Astronomical Institute Groningen October 6, 2011 Overview Types of cataclysmic stars How to form a cataclysmic variable X-ray production Variation in outburst lightcurve,
Supernovae. Supernova basics Supernova types Light Curves SN Spectra after explosion Supernova Remnants (SNRs) Collisional Ionization
Supernovae Supernova basics Supernova types Light Curves SN Spectra after explosion Supernova Remnants (SNRs) Collisional Ionization 1 Supernova Basics Supernova (SN) explosions in our Galaxy and others
4U E. Bozzo. M. Falanga, A. Papitto, L. Stella, R. Perna, D. Lazzati G. Israel, S. Campana, V. Mangano, T. Di Salvo, L.
X-Ray Eclipse Time Delays in 4U2129+47 E. Bozzo M. Falanga, A. Papitto, L. Stella, R. Perna, D. Lazzati G. Israel, S. Campana, V. Mangano, T. Di Salvo, L. Burderi Università di Roma Tor Vergata, Italy
PoS(INTEGRAL 2012)090
XMM-Newton observations of five INTEGRAL sources located towards the Scutum Arm UC Berkeley - Space Sciences Laboratory E-mail: bodaghee@ssl.berkeley.edu John A. Tomsick UC Berkeley - Space Sciences Laboratory
Chapter 14. Outline. Neutron Stars and Black Holes. Note that the following lectures include. animations and PowerPoint effects such as
Note that the following lectures include animations and PowerPoint effects such as fly ins and transitions that require you to be in PowerPoint's Slide Show mode (presentation mode). Chapter 14 Neutron
Compact Stars. Lecture 4
Compact Stars Lecture 4 X-ray binaries We have talked about the basic structure of accretion disks in X-ray binaries and evolutionary scenarios of low mass and high mass XRBs I will now present the observational
Neutrinos and Nucleosynthesis from Black Hole Accretion Disks. Gail McLaughlin North Carolina State University
Neutrinos and Nucleosynthesis from Black Hole Accretion Disks Gail McLaughlin North Carolina State University 1 Neutrino Astrophysics What do neutrinos do in astrophysical environments? What do neutrinos
MULTI-WAVELENGTH OBSERVATIONS OF CYGNUS X-3
MULTI-WAVELENGTH OBSERVATIONS OF CYGNUS X-3 Angelo Varlotta for the VERITAS collaboration Michael McCollough, Wei Cui, Marco Tavani for the AGILE Collaboration, Guy Pooley, Petri Savolainen, Karri Koljonen,
Supernovae. Supernova basics Supernova types Light Curves SN Spectra after explosion Supernova Remnants (SNRs) Collisional Ionization
Supernovae Supernova basics Supernova types Light Curves SN Spectra after explosion Supernova Remnants (SNRs) Collisional Ionization 1 Supernova Basics Supernova (SN) explosions in our Galaxy and others
X-ray emission properties vary with spin-down age. Crab-like pulsars (< 10 4 yrs)
X-ray emission properties vary with spin-down age Crab-like pulsars (< 10 4 yrs) X-ray emission properties vary with spin-down age Crab-like pulsars (< 10 4 yrs) Cooling neutron stars ( ~10 5-10 6 yrs)
Ultra Luminous X-ray sources ~one of the most curious objects in the universe~
Ultra Luminous X-ray sources ~one of the most curious objects in the universe~ Shogo B. Kobayashi the University of Tokyo ULX workshop@isas 1 The discovery of the enigmatic sources pfabbiano & Trincheri
Suzaku observation of the eclipsing high mass X-ray binary pulsar XTE J
J. Astrophys. Astr. (8) 39:7 Indian Academy of Sciences https://doi.org/.7/s36-7-9496-z Suzaku observation of the eclipsing high mass X-ray binary pulsar XTE J8-6 JINCY DEVASIA,, and BISWAJIT PAUL Raman
Anomalous X-ray Pulsars
Anomalous X-ray Pulsars GRBs: The Brightest Explosions in the Universe Harvard University, May 23, 2002 Vicky Kaspi Montreal, Canada What are Anomalous X-ray Pulsars? exotic class of objects 1st discovered
Identification of seven persistent low-luminosity pulsators. Ramanpreet Kaur University of Amsterdam
Identification of seven persistent low-luminosity pulsators Ramanpreet Kaur University of Amsterdam Physics of neutron stars -2011 St Petersburg, Russia Low-luminosity pulsators Slowly pulsating (Ps >
Neutron Stars. Properties of Neutron Stars. Formation of Neutron Stars. Chapter 14. Neutron Stars and Black Holes. Topics for Today s Class
Foundations of Astronomy 13e Seeds Phys1403 Introductory Astronomy Instructor: Dr. Goderya Chapter 14 Neutron Stars and Black Holes Cengage Learning 2016 Topics for Today s Class Neutron Stars What is
arxiv: v1 [astro-ph.sr] 11 Jan 2016
![arxiv: v1 [astro-ph.sr] 11 Jan 2016](/thumbs/92/108440436.jpg "arxiv: v1 [astro-ph.sr] 11 Jan 2016")
Bull. Astr. Soc. India (14) 4,???? arxiv:161.345v1 [astro-ph.sr] 11 Jan 16 Investigation of iron emission lines in the eclipsing high mass X-ray binary pulsar OAO 1657-415 Gaurava K. Jaisawal 1 and Sachindra
The 2006 Outburst of RS Oph: What are the questions that need to be discussed --and answered?
The 2006 Outburst of RS Oph: What are the questions that need to be discussed --and answered? Sumner Starrfield School of Earth and Space Exploration Arizona State University WHY DO WE CARE? RS Oph may
UNIVERSITY of CALIFORNIA SANTA CRUZ
UNIVERSITY of CALIFORNIA SANTA CRUZ VARIABLE X-RAY ABSORPTION IN HIGH-MASS X-RAY BINARIES CYGNUS X-1 AND VELA X-1 A thesis submitted in partial satisfaction of the requirements for the degree of BACHELOR
On the nature of 35-day cycle in Her X-1
On the nature of 35-day cycle in Her X-1 Konstantin Postnov Sternberg Astronomical Institute, Moscow In collaboration with: Ruediger Staubert (IAAT), Nikolai Shakura, Ivan Panchenko (SAI) Joern Wilms (U.
INTEGRAL and RXTE view of Her X-1: towards resolving of the system s puzzles
: towards resolving of the system s puzzles,a, R. Staubert a, K. Postnov b, N. Shakura b, A. Santangelo a, J. Wilms c, and R. Rothschild d a Institut für Astronomie und Astrophysik, Universität Tübingen
Emission from Isolated Neutron Stars. Observations and model applications
Thermal Emission from Isolated Neutron Stars Theoretical aspects Observations and model applications Slava Zavlin (MPE, Garching) A Short History Chi & Salpeter (1964) and Tsuruta (1964): thermal radiation
Supernovae, Neutron Stars, Pulsars, and Black Holes
Supernovae, Neutron Stars, Pulsars, and Black Holes Massive stars and Type II supernovae Massive stars (greater than 8 solar masses) can create core temperatures high enough to burn carbon and heavier
MILLISECOND PULSARS. Merve Çolak
MILLISECOND PULSARS Merve Çolak OUTLINE Corbet Diagram (again) P-P(dot) Diagram MSPs and Their History Properties of MSPs Spin-up of Neutron Stars Spin-down of MSPs MSP Evolution Recent MSP Evolution Model
The Evolution of Close Binaries
The Evolution of Close Binaries Philipp Podsiadlowski (Oxford) The case of RS Ophiuchi as a test of binary stellar evolution as a potential Type Ia supernova (SN Ia) progenitor I. Testing Binary Evolution:
Discovery of a New Gamma-Ray Binary: 1FGL J
Discovery of a New Gamma-Ray Binary: 1FGL J1018.6-5856 Robin Corbet (UMBC/NASA GSFC) on behalf of the Fermi-LAT collaboration, & M.J. Coe, P.G. Edwards, M.D. Filipovic, J.L. Payne, J. Stevens, M.A.P. Torres
PoS(INTEGRAL 2012)089
Results from the first year of the INTEGRAL Spiral Arms Monitoring Program, on behalf of the ISA Collaboration UC Berkeley - Space Sciences Laboratory E-mail: bodaghee@ssl.berkeley.edu The INTEGRAL Spiral
Final States of a Star
Pulsars Final States of a Star 1. White Dwarf If initial star mass < 8 MSun or so. (and remember: Maximum WD mass is 1.4 MSun, radius is about that of the Earth) 2. Neutron Star If initial mass > 8 MSun
arxiv: v1 [astro-ph] 18 Nov 2008
![arxiv: v1 [astro-ph] 18 Nov 2008](/thumbs/90/101828926.jpg "arxiv: v1 [astro-ph] 18 Nov 2008")
Astronomy & Astrophysics manuscript no. sax1818arx c ESO 2018 October 31, 2018 Letter to the Editor Discovery of an eccentric 30 days period in the supergiant X-ray binary SAX J1818.6 1703 with INTEGRAL
Astronomy. Astrophysics. Probing the stellar wind environment of Vela X 1 with MAXI
DOI: 10.1051/0004-6361/201527009 c ESO 2016 Astronomy & Astrophysics Probing the stellar wind environment of Vela X 1 with MAXI C. Malacaria 1,2,T.Mihara 2, A. Santangelo 1,K.Makishima 2,3, M. Matsuoka
A Multiwavelength Study of Cygnus X-1: the First mid-ir Spectroscopic Detection of Compact Jets
Smithsonian Astrophysica A Multiwavelength Study of Cygnus X: the First midir Spectroscopic Detection of Compact Jets F. Rahoui, Harvard University & CfA J.C. Lee, S. Heinz, D.C. Hines, K. Pottschmidt,
Abundance of Elements. Relative abundance of elements in the Solar System
Abundance of Elements Relative abundance of elements in the Solar System What is the origin of elements in the universe? Three elements formed in the first minutes after the big bang (hydrogen, helium
arxiv: v1 [astro-ph.he] 2 Jan 2017
![arxiv: v1 [astro-ph.he] 2 Jan 2017](/thumbs/72/67736439.jpg "arxiv: v1 [astro-ph.he] 2 Jan 2017")
Low-luminosity stellar wind accretion onto neutron stars in HMXBs arxiv:1701.00336v1 [astro-ph.he] 2 Jan 2017 Sternberg Astronomical Institute, Moscow M.V. Lomonosov State University, Universitetskij pr.,
THE FUNDAMENTAL CYCLOTRON LINE IN 4U Introduction
THE FUNDAMENTAL CYCLOTRON LINE IN 4U 1538 52 JOSÉ J. RODES ROCA, JOSÉ M. TORREJÓN, J. GUILLERMO BERNABÉU Departament de Física Enginyeria de Sistemes i Teoria del Senyal, Universitat d Alacant, E-03080
arxiv: v1 [astro-ph.he] 30 Aug 2017
![arxiv: v1 [astro-ph.he] 30 Aug 2017](/thumbs/93/113625039.jpg "arxiv: v1 [astro-ph.he] 30 Aug 2017")
MNRAS, 4 (7) Preprint October 8 Compiled using MNRAS LATEX style file v3. Decade long RXTE monitoring observations of Be/X-ray binary pulsar EXO 3+375 Prahlad Epili, Sachindra Naik, Gaurava K. Jaisawal
Neutron Stars. We now know that SN 1054 was a Type II supernova that ended the life of a massive star and left behind a neutron star.
Neutron Stars Neutron Stars The emission from the supernova that produced the crab nebula was observed in 1054 AD by Chinese, Japanese, Native Americans, and Persian/Arab astronomers as being bright enough
10 Years of Accreting Pulsars with Fermi GBM
https://ntrs.nasa.gov/search.jsp?r=20180007201 2018-11-22T01:58:27+00:00Z 10 Years of Accreting Pulsars with Fermi GBM Colleen A. Wilson-Hodge (NASA/MSFC) Christian Malacaria (NPP/USRA/NASA/MSFC) Peter
Progress in Pulsar detection
Progress in Pulsar detection With EINSTEIN & EXOSAT: 7 radio pulsars detected in X-rays With ROSAT, ASCA & BSAX: 33 radio pulsars detected in X-rays After ~8 yrs with XMM & Chandra: 81 radio pulsars detected
Editorial comment: research and teaching at UT
Wednesday, March 23, 2017 Reading for Exam 3: Chapter 6, end of Section 6 (binary evolution), Section 6.7 (radioactive decay), Chapter 7 (SN 1987A), Background: Sections 3.1, 3.2, 3.3, 3.4, 3.5, 3.8, 3.10,
The Deaths of Stars. The Southern Crab Nebula (He2-104), a planetary nebula (left), and the Crab Nebula (M1; right), a supernova remnant.
The Deaths of Stars The Southern Crab Nebula (He2-104), a planetary nebula (left), and the Crab Nebula (M1; right), a supernova remnant. Once the giant phase of a mediummass star ends, it exhales its outer
Some HI is in reasonably well defined clouds. Motions inside the cloud, and motion of the cloud will broaden and shift the observed lines!
Some HI is in reasonably well defined clouds. Motions inside the cloud, and motion of the cloud will broaden and shift the observed lines Idealized 21cm spectra Example observed 21cm spectra HI densities
High-resolution X-ray Spectroscopy of the Black Hole Cygnus X-1 with the Chandra X-ray observatory
High-resolution X-ray Spectroscopy of the Black Hole Cygnus X-1 with the Chandra X-ray observatory Diploma Thesis Manfred Hanke High-resolution X-ray Spectroscopy of the Black Hole Cygnus X-1 with the
Probing Neutron Star Physics using Thermonuclear X-ray Bursts
Probing Neutron Star Physics using Thermonuclear X-ray Bursts Sudip Bhattacharyya University of Maryland (CRESST) NASA s Goddard Space Flight Center Outline Neutron Stars: why do we care? Thermonuclear
Supergiant Fast X-ray Transients: an INTEGRAL view
Mem. S.A.It. Vol. 83, 251 c SAIt 212 Memorie della Supergiant Fast X-ray Transients: an INTEGRAL view P. Blay 1, I. Negueruela 2, and V. Reglero 1 1 Image Processing Laboratory University of Valencia PO
Rotating RAdio Transients (RRATs) ApJ, 2006, 646, L139 Nature, 2006, 439, 817 Astro-ph/
Rotating RAdio Transients (RRATs) ApJ, 2006, 646, L139 Nature, 2006, 439, 817 Astro-ph/0608311 Introduction 11 Rotating RAdio Transients (RRATs) (Mclaughlin et al 2006) Repeated, irregular radio bursts
V in the outburst of : luminosity dependence of the cyclotron line and pulse profile
Mon. Not. R. Astron. Soc. 371, 19 28 (2006) doi:10.1111/j.1365-2966.2006.10610.x V0332+53 in the outburst of 2004 2005: luminosity dependence of the cyclotron line and pulse profile S. S. Tsygankov, 1,2
(X-ray) binaries in γ-rays
(X-ray) binaries in γ-rays Guillaume Dubus Understanding relativistic jets, Kraków 2011 Institut de Planétologie et d Astrophysique de Grenoble Variable galactic γ-ray sources gamma-ray binaries O/Be +
Monitoring High-Energy Transients with MAXI
Monitoring High-Energy Transients with MAXI Nobuyuki Kawai (Tokyo Tech) on behalf of the MAXI Team Monitor of All-Sky X-ray Image Mission started August 2009 Ops approved until Mar 2018 Real-time link
Astronomy 113. Dr. Joseph E. Pesce, Ph.D. Dr. Joseph E. Pesce, Ph.D.
Astronomy 113 Dr. Joseph E. Pesce, Ph.D. Stellar Deaths/Endpoints 13-2 Low Mass Stars ³ Like the Sun (< 2 M ) ² Live about 10 billion years (sun is middle aged) ² Create elements through Carbon, Nitrogen,
arxiv: v1 [astro-ph.he] 1 Aug 2011
![arxiv: v1 [astro-ph.he] 1 Aug 2011](/thumbs/94/121696283.jpg "arxiv: v1 [astro-ph.he] 1 Aug 2011")
Mon. Not. R. Astron. Soc. 000,???? (2002) Printed 31 October 2018 (MN LATEX style file v2.2) Could AX J1841.0 0536 Be an Anti-Magnetar? X.-D. Li and Z. Zhang Department of Astronomy and Key Laboratory
Interpretation of Early Bursts
Gamma-Ray Bursts Discovery The early years BATSE Fast versus slow bursts Uniformity and log N log S relation BeppoSAX and discovery of afterglows Redshift measurements Connection of long GRBs to supernovae
Neutron Stars. But what happens to the super-dense core? It faces two possible fates:
Neutron Stars When a massive star runs out of fuel, its core collapses from the size of the Earth to a compact ball of neutrons just ten miles or so across. Material just outside the core falls onto this
The fundamental INTEGRAL contributions to advance the millisecond X-ray pulsars research field
The fundamental INTEGRAL contributions to advance the millisecond X-ray pulsars research field M A U R I Z I O F A L A N G A Collaborators: L. Kuipers, W. Hermsen, J. Poutanen, A. Goldwurm, L. Stella June
Dottorato di Ricerca in Astronomia e Astrofisica
UNIVERSITÀ DEGLI STUDI DELL INSUBRIA Facoltà di Scienze Matematiche, Fisiche e Naturali Dottorato di Ricerca in Astronomia e Astrofisica Exploring accretion theory with a new subclass of High Mass X-ray
Analyzing X-Ray Pulses from Stellar Cores Pencil & Paper Version
Analyzing X-Ray Pulses from Stellar Cores Pencil & Paper Version Purpose: To determine if two end products of stellar evolution GK Per and Cen X-3 could be white dwarfs or neutron stars by calculating
Timing Characteristics of the Hard X-ray Emission from Bright X-ray Pulsars Based on INTEGRAL Data
ISSN 163-7737, Astronomy Letters, 29, Vol. 35, No. 7, pp. 433 456. c Pleiades Publishing, Inc., 29. Original Russian Text c A.A. Lutovinov, S.S. Tsygankov, 29, published in Pis ma v Astronomicheskiĭ Zhurnal,
arxiv: v1 [astro-ph.he] 26 Apr 2016
![arxiv: v1 [astro-ph.he] 26 Apr 2016](/thumbs/93/114379906.jpg "arxiv: v1 [astro-ph.he] 26 Apr 2016")
Mon. Not. R. Astron. Soc. 000, 1 6 () Printed 20 October 2018 (MN LATEX style file v2.2) An unexpected drop in the magnetic field of the X-ray pulsar V0332+53 after the bright outburst occurred in 2015
Discovery of a transitional Redback millisecond pulsar J !
Discovery of a transitional Redback millisecond pulsar J1227-4853! By Jayanta Roy!! JBCA, University of Manchester!! and!! National Centre for Radio Astrophysics (NCRA-TIFR) Neutron stars at the crossroads,