New tricks for a mature observatory: Chandra HETG/HRC-I...
Transcript of New tricks for a mature observatory: Chandra HETG/HRC-I...
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New tricks for a mature observatory:
Chandra HETG/HRC-I observations of TW Hya probe
the structure of accretion
Hans Moritz Günther
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Phases of star formation
Artist: McCaughrean
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Classical T Tauri stars
Günther (2013)
Andrews et al.ApJL (2016)
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He-like triplets
Günther et al., A&A (2006)
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The accretion model
● 1D stationary
● optically thin
● no heat conduction
● Maxwell velocity distribution (different temperature for electrons / ions)
● magnetic field does not change dynamics
● non-equilibrium ionisation calculation
Günther et al., A&A (2008)Günther, AN (2011)
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Problems with current models: Accretion interacts with the star
Brickhouse et al. ApJ (2010)Brickhouse et al. ApJ (2012)
Can we resolve the line kinematically?Can we measure time-resolved properties?
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HST/COS
But, what do the X-rays do?
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Multi-wavelength campaign of contemporaneous observations
● Chandra● HST/COS● Magellan/FIRE● FLWO/TRES● El-Trigre● SSO● ...
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HETG/HRC-I: Why?
● ACIS-S contamination increases
● Energies < 1 keV hard to see● LETG has lower resolving
power● HETG/HRC-I might be best
combination for certain science targets:
– Need for best resolution
– Need to lines < 1 keV
– Line dominated spectrum
● No order-sorting– Order confusion– Higher background
(but less than HRC-S)
– HRC-I is flat
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HETG/HRC-I: Status
● NOT a standard product in CIAO <= 4.12
● But can be reduced with CIAO tools with some monkeying
● Working on associated CALDB files, but might require custom RMFs
● MIGHT be fully supported in the future
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TW Hya: Triplets with Chandra
O VII high density r i f
Ne IX: r i f high density
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TW Hya: Changes in density
Ne IX: r i f high density
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● Non-accreting TTS have two component C IV lines (Ardila et al. 2013)
How can we explain the C IV (and other hot ion line) shapes?
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● Pre-shock: freefall velocity
● Post-shock: tubulence, <¼ freefall velocity
How can we explain the C IV (and other hot ion line) shapes?
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● Splatter: turbulent, variablebulk < 100 km/sabsorbtion
How can we explain the C IV (and other hot ion line) shapes?
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● Heated photosphere: 20,000 Kvaries with accretion
How can we explain the C IV (and other hot ion line) shapes?
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C IV line profiles
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Summary
● Use HETG/HRC-I for effective area < 1 keV
● Calibration / data reduction is experimental at this point
● TW Hya has variable f/i ratio
● C IV line profiles can be explained with combination of accretion and outflow