a holy grail for stellar wind analysis zeta puppis seen by xmm
DESCRIPTION
A Holy Grail for stellar wind analysis zeta Puppis seen by XMM. Y. Nazé (FNRS-ULg), G. Rauw (ULg), L. Oskinova (U. Potsdam), E. Gosset (FNRS-ULg), A. Hervé (ULg), C.A. Flores (U. Guanajuato). Zeta Puppis. One of the closest (335pc), earliest (O4I), and brightest massive stars - PowerPoint PPT PresentationTRANSCRIPT
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A Holy Grail for stellar wind A Holy Grail for stellar wind analysis analysis zeta Puppis seen by zeta Puppis seen by
XMMXMM
Y. Nazé (FNRS-ULg), G. Rauw (ULg), Y. Nazé (FNRS-ULg), G. Rauw (ULg), L. Oskinova (U. Potsdam), E. Gosset (FNRS-L. Oskinova (U. Potsdam), E. Gosset (FNRS-
ULg), A. Hervé (ULg), C.A. Flores (U. ULg), A. Hervé (ULg), C.A. Flores (U. Guanajuato)Guanajuato)
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Zeta PuppisZeta Puppis
One of the closest One of the closest (335pc), earliest (O4I), (335pc), earliest (O4I), and brightest massive and brightest massive starsstars
Many intriguing Many intriguing properties : runaway star, properties : runaway star, chemical enrichment, fast chemical enrichment, fast rotation (post RLOF+SN ? rotation (post RLOF+SN ? Ejection from cluster ?)Ejection from cluster ?)
The first one observed by The first one observed by Chandra & XMM Chandra & XMM (Kahn et al. (Kahn et al. 2001, Cassinelli et al. 2011)2001, Cassinelli et al. 2011)
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A decade of XMM A decade of XMM observationsobservations
18 observations18 observations
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Data reductionData reduction
The best dataset available for a massive star The best dataset available for a massive star (~1/2 Ms for EPIC, 3/4 Ms for RGS)(~1/2 Ms for EPIC, 3/4 Ms for RGS)
18 observations taken in different modes (timing, full 18 observations taken in different modes (timing, full frame, large window, small window), with different frame, large window, small window), with different filters (medium, thick), sometimes off-axisfilters (medium, thick), sometimes off-axis
Bright Bright slight pile-up (~limit of large window mode) slight pile-up (~limit of large window mode)
Extraction with pattern=0, keeping the same circular Extraction with pattern=0, keeping the same circular regions for source and bkgd (regions for source and bkgd (NB: annular source = NB: annular source = KO!KO!))
New RGS pipeline (SAS 10) solved the flux/shift issuesNew RGS pipeline (SAS 10) solved the flux/shift issues
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Variability of zeta PuppisVariability of zeta Puppis
In optical : In optical : long-term changes long-term changes (Conti & Niemela 1976)(Conti & Niemela 1976) 5d variations 5d variations (e.g. Moffat & Michaud 1981)(e.g. Moffat & Michaud 1981) a few h pulsations a few h pulsations (e.g. Reid & Howarth 1996)(e.g. Reid & Howarth 1996)
In X-rays : In X-rays : Einstein - nothingEinstein - nothing ROSAT revealed a small modulation (2% ROSAT revealed a small modulation (2%
amplitude) of 17h period in 0.9-2 keV band amplitude) of 17h period in 0.9-2 keV band (Berghöfer et al. 1996)(Berghöfer et al. 1996)
Chandra, XMM (1 dataset) – nothing Chandra, XMM (1 dataset) – nothing (Kahn et al. 2001, Oskinova et al. 2001)(Kahn et al. 2001, Oskinova et al. 2001)
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Variability: Variability: the XMM the XMM
viewview Several energy bandsSeveral energy bands Several time bins (200s Several time bins (200s
to 5ks EPIC, 500s to 10ks to 5ks EPIC, 500s to 10ks RGS)RGS)
Chi-2 tests (constant, Chi-2 tests (constant, line, parabola); Fourier; line, parabola); Fourier; AutocorrelationAutocorrelation
Results :Results : Background is variableBackground is variable Instruments do not agreeInstruments do not agree
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Variability: short & mid-Variability: short & mid-termterm
The longer you The longer you observe or the observe or the longer the time bin, longer the time bin, the more variable it the more variable it is is no obvious short no obvious short term variations but term variations but mid-term ones exist mid-term ones exist (with timescales > (with timescales > Texp : rotation ?)Texp : rotation ?)
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Variability: Variability: short and mid-short and mid-
termterm
For the best data For the best data (small window, thick filter)(small window, thick filter) FourierFourier
0.3-0.4/d + ~1/d ?0.3-0.4/d + ~1/d ? Rotation (5d) ????Rotation (5d) ????
AutocorrelationAutocorrelation >0 if T<20ks, <0 @ 55ks >0 if T<20ks, <0 @ 55ks wind flow time ~5kswind flow time ~5ks
Not very significant anywayNot very significant anyway
Best case : pn dataBest case : pn data
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Variability: linesVariability: lines
RGS dataRGS data TVS : nothingTVS : nothing Count rates and ratios : Count rates and ratios :
nothingnothing Comparison with average Comparison with average
spectrum by eye : non-spectrum by eye : non-significant variations may significant variations may exist but similar to exist but similar to optical…optical…
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VariabilitVariability: long-y: long-
termterm
EPIC, RGS : EPIC, RGS : decrease !decrease !
NB : Fourier, NB : Fourier, autocorrelation and autocorrelation and relative dispersions relative dispersions calculated after calculated after detrendingdetrending
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Variability: long-termVariability: long-term
EPIC spectra : fitted by EPIC spectra : fitted by tbabs (ISM, fixed) tbabs (ISM, fixed) * sum of 4 thermal comp. * sum of 4 thermal comp. (vphabs*vapec – Nh and (vphabs*vapec – Nh and kT fixed)kT fixed)
Pile-up affects all data Pile-up affects all data taken with medium filtertaken with medium filter
Formally unacceptable Formally unacceptable fitting but missing physics fitting but missing physics and disagreement and disagreement between instrumentsbetween instruments
Flux appears quite Flux appears quite constant (a few % constant (a few % decrease?) decrease?) count rate variations count rate variations come from detector come from detector sensitivity changessensitivity changes
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A simple modelA simple model
Features Features (Oskinova et al. (Oskinova et al. 2004)2004) smooth wind or smooth wind or
random absorbersrandom absorbers random emittersrandom emitters solid angle conserved, solid angle conserved,
outward motion (beta outward motion (beta law)law)
LCs less variable:LCs less variable: at high Eat high E for smooth windfor smooth wind For more For more
emitting/absorbing emitting/absorbing clumpsclumps
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How to compare with How to compare with data?data?
Relative dispersions calculated for each Relative dispersions calculated for each observation observation for full LCsfor full LCs for resampled LCsfor resampled LCs
Poisson noise !Poisson noise ! Relative dispersions in both cases ~ Poisson Relative dispersions in both cases ~ Poisson
statistics !statistics !
If additional variability exists, it is hidden in If additional variability exists, it is hidden in noise… hence its amplitude is small, and noise… hence its amplitude is small, and emitting/absorbing clumps are many (>10emitting/absorbing clumps are many (>1055) !) !
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Global spectral fitting : Global spectral fitting : preliminary resultspreliminary results
a a (Kahn et al. 2001, (Kahn et al. 2001, Cassinelli et al. 2011)Cassinelli et al. 2011)
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Line fitting : preliminary Line fitting : preliminary resultsresults
Line profile Line profile fitting using fitting using Owocki & Cohen Owocki & Cohen models : models : variation of tau variation of tau with wavelength with wavelength (cf. Cohen et al. 2010, in (cf. Cohen et al. 2010, in green – NB with resonance green – NB with resonance scattering in red)scattering in red)
BUT /!\ uniqueness BUT /!\ uniqueness of solution…of solution…
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ConclusionsConclusions
A decade of XMM observations = best dataset !A decade of XMM observations = best dataset ! VariabilityVariability
Only noise on short-termOnly noise on short-term Trends on mid-term (DACs ? But no link with rotation, cf. Fourier)Trends on mid-term (DACs ? But no link with rotation, cf. Fourier) Long-term decrease due to detector degradationLong-term decrease due to detector degradation Comparison with models : a lot of wind parcels needed !Comparison with models : a lot of wind parcels needed !
Lines Lines Multi-temperature neededMulti-temperature needed Typical optical depth varies with wavelengthTypical optical depth varies with wavelength
For the future…For the future… Follow the star over its rotation periodFollow the star over its rotation period Observe it with more sensitive detectors to decrease Poisson Observe it with more sensitive detectors to decrease Poisson
noisenoise Develop more detailed modelsDevelop more detailed models