x-ray diagnostics and their relationship to magnetic fields
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X-ray Diagnostics and Their Relationship to Magnetic Fields. David Cohen Swarthmore College. Launched 2000: superior sensitivity, spatial resolution, and spectral resolution. Chandra. XMM-Newton. Sub- arcsecond resolution. - PowerPoint PPT PresentationTRANSCRIPT
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X-ray Diagnostics and Their Relationship to Magnetic Fields
David CohenSwarthmore College
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XMM-Newton
Chandra
Launched 2000: superior sensitivity, spatial resolution, and spectral resolution
Sub-arcsecond resolution
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XMM-Newton
Chandra
Both have CCD detectors for imaging spectroscopy (at low spectral resolution: R~20 to 50)
And – with lower sensitivity – both have grating spectrometers with resolutions of a few 100 to ~1000
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q1 Ori C
Chandra ACISOrion Nebula Cluster (COUP)
Color coded according to photon energy (red: <1keV; green 1 to 2 keV; blue > 2 keV)
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Stelzer et al. 2005
q1 Ori C: X-ray lightcurve
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s Ori E: XMM light curve
Sanz-Forcada et al. 2004
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XMM EPIC spectrum of s Ori E
Sanz-Forcada et al. 2004
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z Pup
q1 Ori C
Si XIIISi XIVMg XIMg XII
Differences between q1 Ori C and a normal O star
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Hot plasma emitting thermal x-rays
1 keV ~ 12 × 106 K ~ 12 Å
ROSAT 150 eV to 2 keVChandra, XMM 500 eV to 10 keV
Shock heating: Dv = 300 km gives T ~ 106 K (and T ~ v2)
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z Pup
q1 Ori C
Chandra grating spectra
q1 Ori C: hotter plasma, narrower emission lines
z Pup: cooler plasma, broad emission lines
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z Pup
q1 Ori C
Si XIIISi XIVMg XIMg XII
H-like/He-like ratio is temperature sensitive
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z Pup
q1 Ori C
Si XIIISi XIVMg XIMg XII
The magnetic O star – q1 Ori C – is hotter
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Differential Emission Measure (temperature distribution)
Wojdowski & Schulz (2005)
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1000 km s-1
Emission lines are significantly narrower, too
q1 Ori C(O7 V)
z Pup(O4 If)
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Wade et al. 2008
Dipole magnetic field
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Recently discovered dipole magnetic field of > 1 kG : Zeeman Doppler spectroscopy (Wade et al. 2006)
Simulation/visualization courtesy R. TownsendMovie available at astro.swarthmore.edu/~cohen/presentations/apip09/rrm-o25-i75-b60-redt.avi
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temperature emission measure
MHD simulations of magnetically channeled wind
Channeled collision is close to head-on – >1000 km s-1 : T > 107 K
simulations by A. ud-Doula; Gagné et al. (2005)
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Differential emission measure (temperature distribution)
MHD simulation of q1 Ori C reproduces the observed
differential emission measureWojdowski & Schulz (2005)
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TRACE
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low-mass stars high-mass stars
Stellar rotation vs. X-ray luminosity
No trend
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High Temperatures – signs of magnetically channeled wind shocks
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But what about magnetic stars with soft X-rays?
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z PupChandra HETGS/MEG spectrum
(R ~ 1000 ~ 300 km s-1)
Si Mg Ne OFe
H-likeHe-like
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What about zeta Ori?
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z Ori: O9.5
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Mg XII Lyman-: * = 0.1
z Ori: O9.5 - less massive
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What about late O and early B stars with big filling factors and
narrow lines?
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Yuri Beletsky (ESO)
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b Crucis aliases:
Mimosa
HD 111123
a massive (16 Msun), luminous (34,000 Lsun), hot (30,000 K) star
…but not quite as hot, massive, and luminous as an O
star: a B0.5 III star
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b Crucis (B0.5 V): lines are narrow!
unresolved
best-fitwind-broadened
Fe XVII line
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b Cru: O VIII Ly- line
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Later-type massive stars with weaker winds… X-ray production is hard to explain…
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Part 2: Magnetically Channeled Winds
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Predictions:
1. Shocks are strong – head-on – and so plasma is hotter;
2. Hot plasma is moving much slower (confinement);
3. Rotational modulation of X-ray flux;4. Hot plasma is ~1 R* above the surface.
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z Pup
q1 Ori C
Chandra grating spectra
q1 Ori C: hotter plasma, narrower emission lines
z Pup: cooler plasma, broad emission lines
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z Pup
q1 Ori C
Si XIIISi XIVMg XIMg XII
H-like/He-like ratio is temperature sensitive
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z Pup
q1 Ori C
Si XIIISi XIVMg XIMg XII
The magnetic O star – q1 Ori C – is hotter
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Differential emission measure (temperature distribution)
MHD simulation of q1 Ori C reproduces the observed
differential emission measureWojdowski & Schulz (2005)
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1000 km s-1
Emission lines are significantly narrower in the magnetic massive star’s x-ray spectrum
q1 Ori C(O7 V)
z Pup(O4 If)
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0.0
0.5
1.0
1.5
Sim
ulat
ion
EM (1
056 c
m-3)
0.0
0.1
0.2
0.3
0.4
θ1 Ori
C A
CIS
-I c
ount
rate
(s-1)
0.0 0.2 0.4 0.6 0.8 1.0Rotational phase (P=15.422 days)
Chandra broadband count rate vs. rotational phase
Model from MHD simulation
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0.0
0.5
1.0
1.5
Sim
ulat
ion
EM (1
056 c
m-3)
0.0
0.1
0.2
0.3
0.4
θ1 Ori
C A
CIS
-I c
ount
rate
(s-1)
0.0 0.2 0.4 0.6 0.8 1.0 Rotational phase (P=15.422 days)
The star itself occults the hot plasma torus
The closer the hot plasma is to
the star, the deeper the dip
in the x-ray light curve
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Emission measure
contour encloses T > 106 K
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Helium-like species’ forbidden-to-intercombination line ratios – z/(x+y) – provide information about the location of the hot plasma
…not the density, as is usually the case.
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g.s. 1s2 1S
1s2s 3S1s2p 3P
1s2p 1P
resonance (w)
intercombination (x+y)forbidden (z)
10-20 eV
1-2 keV
Helium-like ions (e.g. O+6, Ne+8, Mg+10, Si+12, S+14) – schematic energy level diagram
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1s2s 3S1s2p 3P
1s2p 1P
resonance (w)
intercombination (x+y)forbidden (z)
g.s. 1s2 1S
Ultraviolet light from the star’s photosphere drives photoexcitation out of the 3S level
UV
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1s2s 3S1s2p 3P
1s2p 1P
resonance (w)
intercombination (x+y)forbidden (z)
g.s. 1s2 1S
The f/i ratio is thus a diagnostic of the local UV mean intensity…
UV
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1s2s 3S1s2p 3P
1s2p 1P
resonance (w)
intercombination (x+y)forbidden (z)
g.s. 1s2 1S
…and thus the distance of the x-ray emitting plasma from the photosphere
UV
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Rfir=1.2 R*
Rfir=4.0 R*
Rfir=2.1 R*
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He-like f/i ratios and the x-ray light curve both indicate that the hot plasma is somewhat closer to
the photosphere than the MHD models predict.
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Conclusions
Normal massive stars have x-ray line profiles consistent with the predictions of the wind instability model.
Photoelectric absorption’s effect on the profile shapes can be used as a mass-loss rate diagnostic: mass-loss rates are lower than previously thought.
Later-type massive stars have X-rays that are harder to understand, though…
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Conclusions, pt. 2Magnetic massive stars have harder spectra with narrower lines and rotationally modulated variability, in general agreement with MHD simulations.
Line ratio diagnostics are useful for localizing the hot plasma, and indicate that the MHD simulations predict a location that is too far from the photosphere.
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Massive star X-rays vs.
Solar-type X-rays
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YOKOH x-rayfew 106 K
SOHO EUVfew 105 K
Optical5800 K
The Sun at different wavelengths
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rotation convection
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Three models for massive star x-ray emission
1. Instability driven shocks
2. Magnetically channeled wind shocks
3. Wind-wind interaction in close binaries
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Orion’s belt stars
De Martin/Digitized Sky Survey
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Chandra HETGS/MEG spectrum (R ~ 1000 ~ 300 km s-1)
Si Mg NeFe
H-likeHe-like
q1 Ori C
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z Pup
Low-mass star (Capella) for comparison
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z Pup
Capella
Ne X Ne IX Fe XVII
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z Pupmassive
Capellalow mass
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z PupThe x-ray emission lines are broad: agreement with rad hydro simulations
But… they’re also blue shifted and asymmetricIs this predicted by the wind shock scenario?