Formation and Evolution. of the SS 433 Jets. Herman L. Marshall (MIT Kavli Institute) Sebastian Heinz (University Wisconsin)

Size: px
Start display at page:

Download "Formation and Evolution. of the SS 433 Jets. Herman L. Marshall (MIT Kavli Institute) Sebastian Heinz (University Wisconsin)"

Transcription

1 Formation and Evolution Herman L. Marshall (MIT Kavli Institute) Sebastian Heinz (University Wisconsin) Norbert S. Schulz (MIT Kavli Institute) of the SS 433 Jets

2 SS 433 Background Periodically Doppler shifting Hα HeI and Hβ Model: oppositely directed jets at 0.26 c Precession period: 162 days Orbital period: days Radio: verifies model and sets orientation Only jet known to contain baryons Red jet cm Blue jet Blundell & Bowler 2005 Margon et al Texas Symposium Dec 12, /16 Herman L. Marshall SS 433

3 Jet Model Jet is clumped > cm, radio-dominated > cm Clumps move ~ ballistically over x1000 in r Atomic H, He recombination emission at cm Texas Symposium Dec 12, /16 Herman L. Marshall SS 433

4 Two HETGS Spectra Hydrogenic lines Helium-like lines Lines from many ions at 10 7 K < T < 10 8 K Red jet is weak in 1999 but strong in 2001 Lines are broad due to jet expansion Texas Symposium Dec 12, /16 Herman L. Marshall SS 433

5 Jet Model Jet is clumped > cm, radio-dominated > cm Clumps move ~ ballistically over x1000 in r Atomic H, He recombination emission at cm Jet cools from kt > 15 kev Jet contains common metals (from accretion) Jet has constant speed, spreading as it cools Texas Symposium Dec 12, /16 Herman L. Marshall SS 433

6 Trailed Spectra Aug. 8 Made by Doppler Shifting to rest frame Used many lines: Mg XII, Si XIV, Fe XV, etc. Aug. 12 Aug. 16 Aug ,000 Velocity (km/s) 0 Time (ks) -30, ks Texas Symposium Dec 12, /16 Herman L. Marshall SS 433

7 Blue Jet X-ray Spectrum Corrected spectra for time-varying Doppler shifts Combine spectra Ignore red-shifted lines Fit in isis to 4T model Ni: x10 overabundant Texas Symposium Dec 12, /16 Herman L. Marshall SS 433

8 Jet Cooling Model Texas Symposium Dec 12, /16 Herman L. Marshall SS 433

9 Eclipse Spectrum Soft flux doesn t eclipse Texas Symposium Dec 12, /16 Herman L. Marshall SS 433

10 Results from X-ray Data X-ray region cooling time < 5000 s Radiative cooling of thermal plasma < 200 s X-ray emission < 4 x cm (0.05 mas) from shocks that redirect jet and heat gas spectral fit: rmin = 5 x cm, Ljet = 3 x erg/s (Lx ~ ) Jet redirected on 0.2d time scale by 2 Blue, red jets different Perturbed by local effects where jet is directed --> supports a redirection model Eclipsed region spectrum: hard, weak Fe XXV line Most of jet is not eclipsed; > 2 x cm from disk Supports redirection model (or internal shocks) Ni overabundance, enhanced metals --> gas from companion coated with SN products or by jet? Texas Symposium Dec 12, /16 Herman L. Marshall SS 433

11 Jet Model Jet is clumped > cm, radio-dominated > cm Clumps move ~ ballistically over x1000 in r Atomic H, He recombination emission at cm Jet cools from kt > 15 kev Jet contains common metals (from accretion) Jet has constant speed, spreading as it cools Jet is continuous at cm Adiabatic and radiative cooling are comparable Direction is separately set for opposite jets Texas Symposium Dec 12, /16 Herman L. Marshall SS 433

12 Two Shock Geometries Jet starts out baryonic, v~c Model 1: perpendicular shock starts at 20 to disk axis plows through thick accr. disk X-rays visible only on exit Shock zone Accretion Disk Model 2: oblique shock starts out on-axis encounter wind from outer disk can bend jet 20 jet precession due to outer disk Wind Wind Shock zone Texas Symposium Dec 12, /16 Herman L. Marshall SS 433

13 Perpendicular Shock Solutions using Synge EOS Vshock < 0.08c in observed frame kte > 185 kev after shock Texas Symposium Dec 12, /16 Herman L. Marshall SS 433

14 Oblique Shock Model Solve eqns for v2 = 0.26c, θ=20 Eg. Γ1 > 2-3, shock angle = 6-7 Shock is stationary in observed frame Wind Wind Shock zone Texas Symposium Dec 12, /16 Herman L. Marshall SS 433

15 10 12 cm Texas Symposium Dec 12, /16 Herman L. Marshall SS 433

16 Jet Model Jet is clumped > cm, radio-dominated > cm Clumps move ~ ballistically over x1000 in r Atomic H, He recombination emission at cm Jet cools from kt > 15 kev Jet contains common metals (from accretion) Jet has constant speed, spreading as it cools Jet is continuous at cm Adiabatic and radiative cooling are comparable Direction is separately set for opposite jets Shocks likely heat accreted gas to kt > 30 kev Shock model 1: jet intercepts disk funnel Shock model 2: jet bent by wind from outer disk Texas Symposium Dec 12, /16 Herman L. Marshall SS 433

Relativistic Jets from the Black Hole in SS 433

Relativistic Jets from the Black Hole in SS 433 Relativistic Jets from the Black Hole in SS 433 Herman L. Marshall and Laura A. Lopez with Claude R. Canizares, Norbert S. Schulz, and Julie F. Kane MIT Center for Space Research using NASA s Chandra X-ray

More information

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) 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

More information

Deciphering the accretion structure in Vela X-1

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,

More information

Monte Carlo Simulator to Study High Mass X-ray Binary System

Monte Carlo Simulator to Study High Mass X-ray Binary System SLAC-PUB-11350 Monte Carlo Simulator to Study High Mass X-ray Binary System S. Watanabe, F. Nagase, T. Takahashi ISAS/JAXA, Sagamihara, Kanagawa 229-8510, Japan M. Sako, S.M. Kahn KIPAC/Stanford, Stanford,

More information

Spatially Resolved Chandra HETG Spectroscopy of the NLR Ionization Cone in NGC 1068

Spatially Resolved Chandra HETG Spectroscopy of the NLR Ionization Cone in NGC 1068 Spatially Resolved Chandra HETG Spectroscopy of the NLR Ionization Cone in NGC 1068 Dan Evans (MIT Kavli Institute), Patrick Ogle (Caltech), Herman Marshall (MIT), Mike Nowak (MIT), Kim Weaver (GSFC),

More information

MULTIWAVELENGTH OBSERVATIONS OF THE SS 433 JETS

MULTIWAVELENGTH OBSERVATIONS OF THE SS 433 JETS MULTIWAVELENGTH OBSERVATIONS OF THE SS 433 JETS The MIT Faculty has made this article openly available. Please share how this access benefits you. Your story matters. Citation As Published Publisher Marshall,

More information

Dan Evans (Harvard), Julia Lee (Harvard), Jane Turner (UMBC/GSFC), Kim Weaver (GSFC), Herman Marshall (MIT) NGC 2110 Spectroscopy

Dan Evans (Harvard), Julia Lee (Harvard), Jane Turner (UMBC/GSFC), Kim Weaver (GSFC), Herman Marshall (MIT) NGC 2110 Spectroscopy Dan Evans (Harvard), Julia Lee (Harvard), Jane Turner (UMBC/GSFC), Kim Weaver (GSFC), Herman Marshall (MIT) Fe Kα Lines and Reflection: AGN Geometry The Fe Kα line complex in general consists of a narrow

More information

Jets, corona and accretion disk in the black hole source SS433: Monte-Carlo simulations

Jets, corona and accretion disk in the black hole source SS433: Monte-Carlo simulations Jets, corona and accretion disk in the black hole source SS433: Monte-Carlo simulations Yu. M. Krivosheyev, G. S. Bisnovatyi-Kogan,, A. M. Cherepashchuk and K. A. Postnov Space Research Institute of the

More information

Exploring the powering source of the TeV X-ray binary LS 5039

Exploring the powering source of the TeV X-ray binary LS 5039 Exploring the powering source of the TeV X-ray binary LS 5039 Javier Moldón Marc Ribó Josep Maria Paredes Josep Martí (Univ. Jaén) Maria Massi (MPIfR) 9th European VLBI Network Symposium Bologna, Italy

More information

X-ray Radiation, Absorption, and Scattering

X-ray Radiation, Absorption, and Scattering X-ray Radiation, Absorption, and Scattering What we can learn from data depend on our understanding of various X-ray emission, scattering, and absorption processes. We will discuss some basic processes:

More information

Two Flavors of Radio Jets

Two Flavors of Radio Jets Jets Two classes of jets from X-ray binaries Jet power versus accretion power Jet composition Large-scale jets and interactions with ISM Jet production and collimation Two Flavors of Radio Jets Compact

More information

arxiv:astro-ph/ v1 7 Apr 2003

arxiv:astro-ph/ v1 7 Apr 2003 Evidence for Jet Collimation in SS 433 with the Chandra HETGS Masaaki Namiki, 1,2 Nobuyuki Kawai, 1,3 Taro Kotani, 3,4 and Kazuo Makishima 1,5 1 The Institute of Physical and Chemical Research (RIKEN),

More information

X-ray Emission from O Stars. David Cohen Swarthmore College

X-ray Emission from O Stars. David Cohen Swarthmore College X-ray Emission from O Stars David Cohen Swarthmore College Young OB stars are very X-ray X bright L x up to ~10~ 34 ergs s -1 X-ray temperatures: few up to 10+ kev (10s to 100+ million K) K Orion; Chandra

More information

Distribution of X-ray binary stars in the Galaxy (RXTE) High-Energy Astrophysics Lecture 8: Accretion and jets in binary stars

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

More information

AGN Physics of the Ionized Gas Physical conditions in the NLR Physical conditions in the BLR LINERs Emission-Line Diagnostics High-Energy Effects

AGN Physics of the Ionized Gas Physical conditions in the NLR Physical conditions in the BLR LINERs Emission-Line Diagnostics High-Energy Effects AGN Physics of the Ionized Gas Physical conditions in the NLR Physical conditions in the BLR LINERs Emission-Line Diagnostics High-Energy Effects 1 Evidence for Photoionization - continuum and Hβ luminosity

More information

A confirmed stellar-mass ULX with recurrent X-ray occultations from its precessing disk

A confirmed stellar-mass ULX with recurrent X-ray occultations from its precessing disk A confirmed stellar-mass ULX with recurrent X-ray occultations from its precessing disk C. Motch, R. Soria and M. Pakull Thanks to F. Grisé and J. Greiner P13 in NGC 7793 : a key ULX D = 3.7 Mpc In Sculptor

More information

2 The solar atmosphere

2 The solar atmosphere 1 The solar atmosphere 1.1 Introduction The solar atmosphere may be broadly defined as that part of the Sun extending outwards from a level known as the photosphere where energy generated at the Sun s

More information

X-ray Spectroscopy of Massive Star Winds: Shocks, Mass-Loss Rates, and Clumping

X-ray Spectroscopy of Massive Star Winds: Shocks, Mass-Loss Rates, and Clumping X-ray Spectroscopy of Massive Star Winds: Shocks, Mass-Loss Rates, and Clumping David Cohen Department of Physics & Astronomy Swarthmore College Maurice Leutenegger (GSFC), Jon Sundqvist (Madrid), Stan

More information

Randall Smith (CfA) Collaborators: N. Brickhouse, A. Foster, H. Yamaguchi (CfA), J. Wilms (Erlangen), Li Ji (PMO)

Randall Smith (CfA) Collaborators: N. Brickhouse, A. Foster, H. Yamaguchi (CfA), J. Wilms (Erlangen), Li Ji (PMO) Randall Smith (CfA) Collaborators: N. Brickhouse, A. Foster, H. Yamaguchi (CfA), J. Wilms (Erlangen), Li Ji (PMO) X-ray Line Emission from Capella Mg, Si, S, and Fe are unambiguously detected Inconsistent

More information

Extended X- ray emission from PSR B /LS 2883 and other gamma- ray binaries

Extended X- ray emission from PSR B /LS 2883 and other gamma- ray binaries Extended X- ray emission from PSR B1259-63/LS 2883 and other gamma- ray binaries George Pavlov (Pennsylvania State University) Oleg Kargaltsev (George Washington University) Martin Durant (University of

More information

The Chandra Survey of Outflows in AGN with Resolved Spectroscopy (SOARS)

The Chandra Survey of Outflows in AGN with Resolved Spectroscopy (SOARS) The Chandra Survey of Outflows in AGN with Resolved Spectroscopy (SOARS) Dan Evans (CfA and Elon University) Kevin Schawinski (Yale), Francisco Muller Sanchez (IAC/UCLA), Herman Marshall (MIT), Martin

More information

GRB history. Discovered 1967 Vela satellites. classified! Published 1973! Ruderman 1974 Texas: More theories than bursts!

GRB history. Discovered 1967 Vela satellites. classified! Published 1973! Ruderman 1974 Texas: More theories than bursts! Discovered 1967 Vela satellites classified! Published 1973! GRB history Ruderman 1974 Texas: More theories than bursts! Burst diversity E peak ~ 300 kev Non-thermal spectrum In some thermal contrib. Short

More information

WHAT DO X-RAY OBSERVATIONS

WHAT DO X-RAY OBSERVATIONS WHAT DO X-RAY OBSERVATIONS OF SNRS TELL US ABOUT THE SN AND ITS PROGENITOR DAN PATNAUDE (SAO) ANATOMY OF A SUPERNOVA REMNANT Forward Shock Cas A viewed in X-rays (Patnaude & Fesen 2009). Red corresponds

More information

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 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

More information

Extended X-ray object ejected from the PSR B /LS 2883 binary

Extended X-ray object ejected from the PSR B /LS 2883 binary Extended X-ray object ejected from the PSR B1259-63/LS 2883 binary Oleg Kargaltsev (George Washington University) George Pavlov (Pennsylvania State University) Jeremy Hare (George Washington University)

More information

X-ray spectroscopy of nearby galactic nuclear regions

X-ray spectroscopy of nearby galactic nuclear regions X-ray spectroscopy of nearby galactic nuclear regions 1. How intermittent are AGNs? 2. What about the silent majority of the SMBHs? 3. How do SMBHs interplay with their environments? Q. Daniel Wang University

More information

V5116 Sgr (Nova Sgr 2005b): an eclipsing supersoft postoutburst nova?

V5116 Sgr (Nova Sgr 2005b): an eclipsing supersoft postoutburst nova? V5116 Sgr (Nova Sgr 2005b): an eclipsing supersoft postoutburst nova? (UPC-IEEC, Barcelona) Margarita Hernanz, Carlo Ferri (CSIC-IEEC, Barcelona) Jochen Greiner (MPE, Garching) X-ray emission from Classical

More information

X-ray Radiation, Absorption, and Scattering

X-ray Radiation, Absorption, and Scattering X-ray Radiation, Absorption, and Scattering What we can learn from data depend on our understanding of various X-ray emission, scattering, and absorption processes. We will discuss some basic processes:

More information

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 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

More information

AGN Outflows in Dynamic ICMs: Winds and Twists

AGN Outflows in Dynamic ICMs: Winds and Twists AGN Outflows in Dynamic ICMs: Winds and Twists Tom Jones University of Minnesota Pete Mendygral (UMN, Cray Computer) David Porter (UMN) Klaus Dolag (MPA, U Munich) 11/29/2012 Binary Black Holes & Dual

More information

Hot-subdwarf stars: a new class of X-ray sources

Hot-subdwarf stars: a new class of X-ray sources Hot-subdwarf stars: a new class of X-ray sources Nicola La Palombara 1 S. Mereghetti 1, A. Tiengo 1,2,3, P. Esposito 1 1 INAF - IASF Milano, 2 IUSS Pavia, 3 INFN Pavia Dublin June 16-19, 2014 Hot subdwarf

More information

AGN Central Engines. Supermassive Black Holes (SMBHs) Masses and Accretion Rates SMBH Mass Determinations Accretion Disks

AGN Central Engines. Supermassive Black Holes (SMBHs) Masses and Accretion Rates SMBH Mass Determinations Accretion Disks AGN Central Engines Supermassive Black Holes (SMBHs) Masses and Accretion Rates SMBH Mass Determinations Accretion Disks 1 Supermassive Black Holes Need to generate L > 10 43 ergs/sec inside radius < 10

More information

X-ray spectroscopy of low-mass X-ray binaries

X-ray spectroscopy of low-mass X-ray binaries X-ray spectroscopy of low-mass X-ray binaries Laurence Boirin Observatoire astronomique de Strasbourg (Handout version) Artistic impression of a low-mass X-ray binary An X-ray binary spectrum (from the

More information

Development of multilayer mirror based soft X-ray polarimeter

Development of multilayer mirror based soft X-ray polarimeter Development of multilayer mirror based soft X-ray polarimeter S.S.Panini (IIA), P. Sreekumar (IIA), Herman L Marshall (MIT Kavli), Shyama Narendranath (ISRO), M. Nayak (RRCAT), P.S.Athiray (University

More information

The Non Equilibrium Ionization Model in ISIS

The Non Equilibrium Ionization Model in ISIS The Non Equilibrium Ionization Model in ISIS L. Ji1, N.S. Schulz1, M. Nowak1, H.L. Marshall1, M. Noble1, J. Kwan2 1 MIT Kavli Institute for Astrophysics and Space Research 2 University of Massachusettes,

More information

Physics of the hot evolving Universe

Physics of the hot evolving Universe Physics of the hot evolving Universe Science themes for a New-Generation X-ray Telescope Günther Hasinger Max-Planck-Institut für extraterrestrische Physik Garching ESA Cosmic Vision 2015-2025 Workshop,

More information

MULTI-WAVELENGTH OBSERVATIONS OF CYGNUS X-3

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,

More information

A Detailed Study of. the Pulsar Wind Nebula 3C 58

A Detailed Study of. the Pulsar Wind Nebula 3C 58 A Detailed Study of Collaborators: D. J. Helfand S. S. Murray S. Ransom F. D. Seward B. M. Gaensler E. V. Gotthelf E. van der Swaluw the Pulsar Wind Nebula 3C 58 Pulsar Wind Nebulae Young NS powers a particle/magnetic

More information

Isolated And Accreting Magnetars Viewed In Hard X-rays

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

More information

Astrophysical Quantities

Astrophysical Quantities Astr 8300 Resources Web page: http://www.astro.gsu.edu/~crenshaw/astr8300.html Electronic papers: http://adsabs.harvard.edu/abstract_service.html (ApJ, AJ, MNRAS, A&A, PASP, ARAA, etc.) General astronomy-type

More information

Probing Neutron Star Physics using Thermonuclear X-ray Bursts

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

More information

Decretion Disk Dynamics in Binary Be Stars

Decretion Disk Dynamics in Binary Be Stars Decretion Disk Dynamics in Binary Be Stars Atsuo Okazaki (Hokkai- Gakuen Univ, Japan) In collaboration with S. Stefl (ESO), Th. Rivinius (ESO), D. Baade (ESO), K. Hayasaki (Hokkaido Univ, Japan) 1 Talk

More information

Stellar Winds. Star. v w

Stellar Winds. Star. v w Stellar Winds Star v w Stellar Winds Geoffrey V. Bicknell 1 Characteristics of stellar winds Solar wind Velocity at earth s orbit: Density: Temperature: Speed of sound: v 400 km/s n 10 7 m 3 c s T 10 5

More information

4U E. Bozzo. M. Falanga, A. Papitto, L. Stella, R. Perna, D. Lazzati G. Israel, S. Campana, V. Mangano, T. Di Salvo, L.

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

More information

PHOTOIONIZATION X-RAY BINARIES INSTABILITY OF WINDS IN STEFANO BIANCHI. June 8 th 2017 The X-ray Universe 2017 Rome, Italy

PHOTOIONIZATION X-RAY BINARIES INSTABILITY OF WINDS IN STEFANO BIANCHI. June 8 th 2017 The X-ray Universe 2017 Rome, Italy PHOTOIONIZATION INSTABILITY OF WINDS IN X-RAY BINARIES STEFANO BIANCHI June 8 th 2017 The X-ray Universe 2017 Rome, Italy 4U1630-472 Suzaku WINDS IN GBHS GROJ1655-40 XMM Kubota+ 07 Diaz-Trigo+ 07 WINDS

More information

Afterglows Theory Re em Sari - Caltech

Afterglows Theory Re em Sari - Caltech Π= Π m /3 Afterglows Theory Re em Sari - Caltech 30s 2h t -2 30m t +1/2 t Rising -1 spectrum ν 1/3 1d t -2.2 100d t -1.5 Gamma-Ray Burst: 4 Stages 1) Compact Source, E>10 51 erg 2) Relativistic Kinetic

More information

K. Atapin, S. Fabrika

K. Atapin, S. Fabrika K. Atapin, S. Fabrika Strasbourg - 2016 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

More information

Connections between Radio and High Energy Emission in AGN

Connections between Radio and High Energy Emission in AGN Connections between Radio and High Energy Emission in AGN Geoff Bicknell Research School of Astronomy & Astrophysics Australian National University 1 Collaborators: Loredana Bassani, INAF, Bologna Nadine

More information

Line Profile Variability in AGNs

Line Profile Variability in AGNs Line Profile Variability in AGNs Wolfram Kollatschny, Göttingen Serbia, 2007 University Observatory Institute for Astrophysics Scale Sizes of an AGN HST : 0.1 2pc R. Blandford 1pc = 3.3 ly = 1190. ld =

More information

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 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

More information

Study of Electron Energy and Angular Distributions and Calculations of X-ray, EUV Line Flux and Rise Times

Study of Electron Energy and Angular Distributions and Calculations of X-ray, EUV Line Flux and Rise Times J. Astrophys. Astr. (1987) 8, 263 270 Study of Electron Energy and Angular Distributions and Calculations of X-ray, EUV Line Flux and Rise Times Ranjna Bakaya, Sunil Peshin, R. R. Rausaria & P. N. Khosa

More information

SUPERNOVA REMNANT 1987A: HIGH RESOLUTION IMAGES AND SPECTRUM FROM CHANDRA OBSERVATIONS

SUPERNOVA REMNANT 1987A: HIGH RESOLUTION IMAGES AND SPECTRUM FROM CHANDRA OBSERVATIONS 1 SUPERNOVA REMNANT 1987A: HIGH RESOLUTION IMAGES AND SPECTRUM FROM CHANDRA OBSERVATIONS S. Park 1, S. A. Zhekov 2,4, D. N. Burrows 1, J. L. Racusin 1, R. McCray 2, and K. J. Borkowski 3 1 Department of

More information

Modeling Non-Equilbirum Plasma. Adam Foster

Modeling Non-Equilbirum Plasma. Adam Foster Modeling Non-Equilbirum Plasma Adam Foster Definition CIE plasma: a plasma which is in collisional ionization equilibrium NEI plasma: a collisional plasma which is not in CIE Ionization Balance dn ( z)

More information

NUCLEOSYNTHESIS INSIDE GAMMA-RAY BURST ACCRETION DISKS AND ASSOCIATED OUTFLOWS

NUCLEOSYNTHESIS INSIDE GAMMA-RAY BURST ACCRETION DISKS AND ASSOCIATED OUTFLOWS NUCLEOSYNTHESIS INSIDE GAMMA-RAY BURST ACCRETION DISKS AND ASSOCIATED OUTFLOWS Indrani Banerjee Indian Institute of Science Bangalore The work has been done in collaboration with Banibrata Mukhopadhyay

More information

Thermal pressure vs. magnetic pressure

Thermal pressure vs. magnetic pressure Thermal pressure vs. magnetic pressure The Earth The auroral oval: bremsstrahlung and lines induced by electrons precipitating through the Earth s magnetic field (LX ~ 10 14 erg/s ~ 2 kg TNT equivalent/s)

More information

Introduction to AGN. General Characteristics History Components of AGN The AGN Zoo

Introduction to AGN. General Characteristics History Components of AGN The AGN Zoo Introduction to AGN General Characteristics History Components of AGN The AGN Zoo 1 AGN What are they? Active galactic nucleus compact object in the gravitational center of a galaxy that shows evidence

More information

Accretion Disks. 1. Accretion Efficiency. 2. Eddington Luminosity. 3. Bondi-Hoyle Accretion. 4. Temperature profile and spectrum of accretion disk

Accretion Disks. 1. Accretion Efficiency. 2. Eddington Luminosity. 3. Bondi-Hoyle Accretion. 4. Temperature profile and spectrum of accretion disk Accretion Disks Accretion Disks 1. Accretion Efficiency 2. Eddington Luminosity 3. Bondi-Hoyle Accretion 4. Temperature profile and spectrum of accretion disk 5. Spectra of AGN 5.1 Continuum 5.2 Line Emission

More information

Shock Waves. = 0 (momentum conservation)

Shock Waves. = 0 (momentum conservation) PH27: Aug-Dec 2003 Shock Waves A shock wave is a surface of discontinuity moving through a medium at a speed larger than the speed of sound upstream. The change in the fluid properties upon passing the

More information

Transient iron fluorescence: new clues on the AGN disk/corona?

Transient iron fluorescence: new clues on the AGN disk/corona? Transient iron fluorescence: new clues on the AGN disk/corona? Emanuele Nardini Horizon 2020 INAF/Arcetri AstroFIt2/MSCA in collaboration with: D. Porquet (CNRS/Strasbourg), J. Reeves (Keele+UMBC), V.

More information

Balmer- and L-shell series of highly charged uranium in the experimental storage ring

Balmer- and L-shell series of highly charged uranium in the experimental storage ring Balmer- and L-shell series of highly charged uranium in the experimental storage ring Summer student program @ GSI - 2007 Thomas Burschil Johann Wolfgang von Goethe-University, Frankfurt/Main 09/24/2007

More information

Radiative Processes in Astrophysics

Radiative Processes in Astrophysics Radiative Processes in Astrophysics 11. Synchrotron Radiation & Compton Scattering Eline Tolstoy http://www.astro.rug.nl/~etolstoy/astroa07/ Synchrotron Self-Absorption synchrotron emission is accompanied

More information

GRB : Modeling of Multiwavelength Data

GRB : Modeling of Multiwavelength Data GRB 090510: Modeling of Multiwavelength Data Soeb Razzaque NRC-NRL, Washington, DC Gamma Ray Bursts Workshop, Nov 8-12, GSFC Detection of GRB 090510 Fermi GBM and LAT observations Trigger on 2009 May 10

More information

Francesco Tombesi. University of Rome, Tor Vergata NASA - Goddard Space Flight Center University of Maryland, College Park

Francesco Tombesi. University of Rome, Tor Vergata NASA - Goddard Space Flight Center University of Maryland, College Park Francesco Tombesi University of Rome, Tor Vergata NASA - Goddard Space Flight Center University of Maryland, College Park (credit JAXA s press release) Warm Absorbers (WAs) (Photo) ionized Mrk 509 v~300-800

More information

Nuclear X-ray Emission and Mass Outflow From Broad Lined Radio Galaxies (Lorentz Center, Leiden 2009)

Nuclear X-ray Emission and Mass Outflow From Broad Lined Radio Galaxies (Lorentz Center, Leiden 2009) Nuclear X-ray Emission and Mass Outflow From Broad Lined Radio Galaxies (Lorentz Center, Leiden 2009) James Reeves (Keele Univ, UK) Collaborators:- Rita Sambruna (NASA/GSFC), Francesco Tombesi (NASA/GSFC

More information

AG Draconis. A high density plasma laboratory. Dr Peter Young Collaborators A.K. Dupree S.J. Kenyon B. Espey T.B.

AG Draconis. A high density plasma laboratory. Dr Peter Young Collaborators A.K. Dupree S.J. Kenyon B. Espey T.B. AG Draconis A high density plasma laboratory Collaborators A.K. Dupree S.J. Kenyon B. Espey T.B. Ake p.r.young@rl.ac.uk Overview CHIANTI database Symbiotic Stars AG Draconis FUSE FUSE observations of AG

More information

MASSACHUSETTS INSTITUTE OF TECHNOLOGY Physics Department Earth, Atmospheric, and Planetary Sciences Department. Final Exam

MASSACHUSETTS INSTITUTE OF TECHNOLOGY Physics Department Earth, Atmospheric, and Planetary Sciences Department. Final Exam MASSACHUSETTS INSTITUTE OF TECHNOLOGY Physics Department Earth, Atmospheric, and Planetary Sciences Department Physics 8.282J EAPS 12.402J May 20, 2005 Final Exam Name Last First (please print) 1. Do any

More information

The Physics and Dynamics of Planetary Nebulae

The Physics and Dynamics of Planetary Nebulae Grigor A. Gurzadyan The Physics and Dynamics of Planetary Nebulae With 125 Figures, 14 Plates and 93 Tables Springer Contents 1. Global Concepts 1 1.1 The Shapes of Planetary Nebulae 1 1.2 The Structure

More information

Influence of Mass Flows on the Energy Balance and Structure of the Solar Transition Region

Influence of Mass Flows on the Energy Balance and Structure of the Solar Transition Region **TITLE** ASP Conference Series, Vol. **VOLUME***, **YEAR OF PUBLICATION** **NAMES OF EDITORS** Influence of Mass Flows on the Energy Balance and Structure of the Solar Transition Region E. H. Avrett and

More information

X-ray data analysis. Andrea Marinucci. Università degli Studi Roma Tre

X-ray data analysis. Andrea Marinucci. Università degli Studi Roma Tre X-ray data analysis Andrea Marinucci Università degli Studi Roma Tre marinucci@fis.uniroma3.it Goal of these lectures X-ray data analysis why? what? how? Why? Active Galactic Nuclei (AGN) Physics in a

More information

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 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

More information

Unraveling the Origin of Overionized Plasma in the Galactic Supernova Remnant W49B

Unraveling the Origin of Overionized Plasma in the Galactic Supernova Remnant W49B Unraveling the Origin of Overionized Plasma in the Galactic Supernova Remnant W49B Sarah Pearson (University of Copenhagen) 3 January 2013 In collaboration with: Laura A. Lopez (MIT), Enrico Ramirez-Ruiz

More information

Discovery of Emission Lines in the X-ray Spectrum of the Perseus Cluster

Discovery of Emission Lines in the X-ray Spectrum of the Perseus Cluster Discovery of Emission Lines in the X-ray Spectrum of the Perseus Cluster J. L. Culhane University College London Mullard Space Science Laboratory Summary Nature of the Solar Corona and properties of its

More information

Multi-wavelength Observations of Colliding Stellar Winds

Multi-wavelength Observations of Colliding Stellar Winds Multi-wavelength Observations of Colliding Stellar Winds Mike Corcoran Universities Space Research Association and NASA/GSFC Laboratory for High Energy Astrophysics Collaborators: Julian Pittard (Leeds)

More information

Stellar Populations: Resolved vs. unresolved

Stellar Populations: Resolved vs. unresolved Outline Stellar Populations: Resolved vs. unresolved Individual stars can be analyzed Applicable for Milky Way star clusters and the most nearby galaxies Integrated spectroscopy / photometry only The most

More information

Neutron star mass and radius constraints from X-ray bursts, accreting millisecond pulsars and X-ray polarization. Juri Poutanen

Neutron star mass and radius constraints from X-ray bursts, accreting millisecond pulsars and X-ray polarization. Juri Poutanen Neutron star mass and radius constraints from X-ray bursts, accreting millisecond pulsars and X-ray polarization Juri Poutanen University of Turku, Finland Nordita, Stockholm, Sweden Collaborators: Joonas

More information

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? 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

More information

Plumes as seen in the Ultraviolet

Plumes as seen in the Ultraviolet Plumes as seen in the Ultraviolet L. Teriaca Max Planck Institut für Sonnensystemforschung Introduction Plumes have been observed and studied since long time in white light during total eclipses (Abbot

More information

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/ 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

More information

RELATIVISTIC SPECTROSCOPY OF BLACK HOLES

RELATIVISTIC SPECTROSCOPY OF BLACK HOLES RELATIVISTIC SPECTROSCOPY OF BLACK HOLES Michael Parker ESAC science seminar 24/5/18 BLACK HOLES 101 For an object to just escape a massive body, it needs the sum: Kinetic energy + gravitational binding

More information

Basics, types Evolution. Novae. Spectra (days after eruption) Nova shells (months to years after eruption) Abundances

Basics, types Evolution. Novae. Spectra (days after eruption) Nova shells (months to years after eruption) Abundances Basics, types Evolution Novae Spectra (days after eruption) Nova shells (months to years after eruption) Abundances 1 Cataclysmic Variables (CVs) M.S. dwarf or subgiant overflows Roche lobe and transfers

More information

Winds and X-ray reverberation in AGN

Winds and X-ray reverberation in AGN Winds and X-ray reverberation in AGN Jane Turner (UMBC) James Reeves (Keele) Valentina Braito (Leicester) Andrew Lobban (Keele) Stuart Sim (MPA) Knox Long (STScI) Daniel Proga (Nevada) Steve Kraemer (Catholic)

More information

X-ray Outbursts from Black Hole Binaries. Ron Remillard Center for Space Research, MIT

X-ray Outbursts from Black Hole Binaries. Ron Remillard Center for Space Research, MIT X-ray Outbursts from Black Hole Binaries Ron Remillard Center for Space Research, MIT Outline Status Report on Black Hole Binaries X-ray States of Accreting Black Holes Modified State Definitions Outline

More information

NuSTAR spectral analysis of the two bright Seyfert 1 galaxies: MCG and NGC Alessia Tortosa Università Roma Tre

NuSTAR spectral analysis of the two bright Seyfert 1 galaxies: MCG and NGC Alessia Tortosa Università Roma Tre NuSTAR spectral analysis of the two bright Seyfert 1 galaxies: MCG 8-11-11 and NGC 6814 Alessia Tortosa Università Roma Tre From the Dolomites to the event horizon: sledging down the black hole potential

More information

Pulsar Wind Nebulae. Pennsylvania State University. General outlook Chandra results Polarization in radio and optical X-ray polarization

Pulsar Wind Nebulae. Pennsylvania State University. General outlook Chandra results Polarization in radio and optical X-ray polarization Pulsar Wind Nebulae George Pavlov & Oleg Kargaltsev Pennsylvania State University General outlook Chandra results Polarization in radio and optical X-ray polarization Pulsar Wind Nebulae: extended objects

More information

Atomic Structure & Radiative Transitions

Atomic Structure & Radiative Transitions Atomic Structure & Radiative Transitions electron kinetic energy nucleus-electron interaction electron-electron interaction Remember the meaning of spherical harmonics Y l, m (θ, ϕ) n specifies the

More information

Halo Gas Velocities Using Multi-slit Spectroscopy

Halo Gas Velocities Using Multi-slit Spectroscopy Halo Gas Velocities Using Multi-slit Spectroscopy Cat Wu Thesis Proposal, Fall 2009 Astronomy Department New Mexico State University Outline Diffuse ionized gas; galaxy halos Origin of halo galactic fountain

More information

Sequence Obs ID Instrument Exposure uf Exposure f Date Observed Aimpoint (J2000) (ks) (ks) (α, δ)

Sequence Obs ID Instrument Exposure uf Exposure f Date Observed Aimpoint (J2000) (ks) (ks) (α, δ) 1 SUMMARY 1 G120.1+01.4 1 Summary Common Name: Tycho s Distance: 2.4 kpc ( Chevalier et al., 1980 ) Center of X-ray emission (J2000): ( 00 25 19.9, 64 08 18.2 ) X-ray size: 8.7 x8.6 Description: 1.1 Summary

More information

X-raying galactic feedback in nearby disk galaxies. Q. Daniel Wang University of Massachusetts

X-raying galactic feedback in nearby disk galaxies. Q. Daniel Wang University of Massachusetts X-raying galactic feedback in nearby disk galaxies Q. Daniel Wang University of Massachusetts Chandra survey of diffuse X-ray emission from 53 edge-on galaxies i > 60 o, D < 30 Mpc (Li, J.-T. & Wang, Q.D.

More information

ACTIVE GALACTIC NUCLEI: FROM THE CENTRAL BLACK HOLE TO THE GALACTIC ENVIRONMENT

ACTIVE GALACTIC NUCLEI: FROM THE CENTRAL BLACK HOLE TO THE GALACTIC ENVIRONMENT Julian H. Krolik ACTIVE GALACTIC NUCLEI: FROM THE CENTRAL BLACK HOLE TO THE GALACTIC ENVIRONMENT PRINCETON UNIVERSITY PRESS Princeton, New Jersey Preface Guide for Readers xv xix 1. What Are Active Galactic

More information

High-Energy Astrophysics Lecture 6: Black holes in galaxies and the fundamentals of accretion. Overview

High-Energy Astrophysics Lecture 6: Black holes in galaxies and the fundamentals of accretion. Overview High-Energy Astrophysics Lecture 6: Black holes in galaxies and the fundamentals of accretion Robert Laing Overview Evidence for black holes in galaxies and techniques for estimating their mass Simple

More information

Lecture 20 High-Energy Astronomy. HEA intro X-ray astrophysics a very brief run through. Swift & GRBs 6.4 kev Fe line and the Kerr metric

Lecture 20 High-Energy Astronomy. HEA intro X-ray astrophysics a very brief run through. Swift & GRBs 6.4 kev Fe line and the Kerr metric Lecture 20 High-Energy Astronomy HEA intro X-ray astrophysics a very brief run through. Swift & GRBs 6.4 kev Fe line and the Kerr metric Tut 5 remarks Generally much better. However: Beam area. T inst

More information

Modeling Compton Thick Obscuration in Accreting Supermassive Black Hole Systems

Modeling Compton Thick Obscuration in Accreting Supermassive Black Hole Systems Modeling Compton Thick Obscuration in Accreting Supermassive Black Hole Systems Kendrah Murphy MIT Kavli Institute for Astrophysics & Space Research Tahir Yaqoob Johns Hopkins University/NASA GSFC Overview

More information

Origin of the Galactic Ridge X-ray Emission (GRXE) unresolved

Origin of the Galactic Ridge X-ray Emission (GRXE) unresolved Origin of the Galactic Ridge X-ray Emission (GRXE) unresolved Ken Ebisawa (JAXA/ISAS) Kumiko Morihana (Nishiharima Astronomical Observatory) Masahiro Tsujimoto (JAXA/ISAS) 1 Contents 1. Introduction and

More information

Black Holes and Active Galactic Nuclei

Black Holes and Active Galactic Nuclei Black Holes and Active Galactic Nuclei A black hole is a region of spacetime from which gravity prevents anything, including light, from escaping. The theory of general relativity predicts that a sufficiently

More information

The simulated 21 cm signal during the EoR : Ly-α and X-ray fluctuations

The simulated 21 cm signal during the EoR : Ly-α and X-ray fluctuations The simulated 21 cm signal during the EoR : Ly-α and X-ray fluctuations Sunghye BAEK Collaborators : B. Semelin, P. Di Matteo, F. Combes, Y. Revaz LERMA - Observatoire de Paris 9 Dec 2008 Physics of the

More information

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. 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

More information

Citation for published version (APA): Wang, Y. (2018). Disc reflection in low-mass X-ray binaries. [Groningen]: Rijksuniversiteit Groningen.

Citation for published version (APA): Wang, Y. (2018). Disc reflection in low-mass X-ray binaries. [Groningen]: Rijksuniversiteit Groningen. University of Groningen Disc reflection in low-mass X-ray binaries Wang, Yanan IMPORTANT NOTE: You are advised to consult the publisher's version (publisher's PDF) if you wish to cite from it. Please check

More information

A Suzaku, NuSTAR, and XMM-Newton view on variable absorption and relativistic reflection in NGC 4151

A Suzaku, NuSTAR, and XMM-Newton view on variable absorption and relativistic reflection in NGC 4151 A Suzaku, NuSTAR, and XMM-Newton view on variable absorption and relativistic reflection in NGC 411 T. Beuchert, A.G. Markowitz, T. Dauser, J.A. García, M.L. Keck, J. Wilms, M. Kadler, L.W. Brenneman,

More information

Roberto Soria (UCAS) Jets and outflows from super-eddington sources

Roberto Soria (UCAS) Jets and outflows from super-eddington sources Jets and outflows from super-eddington sources Roberto Soria (UCAS) Also thanks to: Ryan Urquhart (ICRAR PhD student) James Miller-Jones (ICRAR-Curtin) Manfred Pakull (Strasbourg Observatory) Christian

More information

The high-energy view of Seyfert galaxies through broad-band monitoring campaigns

The high-energy view of Seyfert galaxies through broad-band monitoring campaigns The high-energy view of Seyfert galaxies through broad-band monitoring campaigns Francesco Ursini INAF-Osservatorio di Astrofisica e Scienza dello Spazio di Bologna In collaboration with: P.-O. Petrucci,

More information