Studying Protostellar and Debris Disks with BLISS

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Studying Protostellar and Debris Disks with BLISS

• Harold W. Yorke
• Harold.Yorke_at_jpl.nasa.gov
• Presented at
• BLISS Kick-off
• JPL, September 10, 2004

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How can BLISS enhance star formation Science?
(1/2)

• General Comments
• Dust continuum emission peaks in FIR/submm out to
  z lt 5
• Many important molecular fine structure lines
  not available from ground (HD, H2O/HDO, OH,
  fs-lines, bending modes of hot complex molecules,
  high-J CO)
• Submm atmospheric windows do not permit access
  to all needed diagnostic lines at a given
  redshift
• 3 12µm PAH features shift into FIR window
  beyond z gt 7
• Stars, Disks, and Planets
• Structure and characterization of circumstellar
  disks before, during and after planet-forming
  stages
• Detection and mapping of large (pre-biotic?)
  molecules
• Characterize the dust during evolution using FIR
  features
• Other science jets and outflows including
  dust-producing evolved stars, structure and
  kinematics of molecular clouds and Galactic
  Center region

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How can BLISS enhance star formation Science?
(2/2)

• Star Formation Activity within nearby Galaxies (1
  kpc spatial resolution or better)
• ISM properties as a function of location
  (temperature, density, metallicity, uv radiation
  hardness and density).
• Star formation rate from PDR activity as a
  function of location (spiral arms, nuclear
  starburst, etc...) and of local ISM conditions
• Influence of neighboring galaxies on SFR and ISM
  properties.
• Star Formation History
• Population III stars form via HD and H2 cooling
  of metalless clouds
• PAH features and fs diagnostic lines can be used
  out to reionization epoch to
• Disentangle AGN activity versus Starburst
  activity
• Study metalicity history

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Emission from Star Forming Regions
Dusty galaxies emit mostly in the far-IR. These
wave-lengths probe their star formation
properties and evolution
Emission from a star forming region (70K) with
spectral lines imposed on the dust continuum.
CII at 158 µm, the strongest cooling line in the
ISM. BICE Galactic maps of CII at very low
spectral resolution (top) and dust emission
(bottom).
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Important relevant time scales

• Free-fall time scale
• Accretion time scale
• Kelvin-Helmholtz time scale (time to reach ZAMS)

M -2
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Accretion and mass loss as mass exchange between
components
Cloud Clump Core
Jets and Outflows
load
acc
S-wind
D-wind
Disk can act as reservoir for material
Star
Disk
disk
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Dynamical Models of Protostellar Disks
(Yorke Bodenheimer 1999, ApJ, 525, 330)
2 MO ? r -2
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Dynamical Models of Protostellar Disks
(Yorke Bodenheimer 1999, ApJ, 525, 330)
2 MO ? r -2
SEDs as a function of time and orientation (0O,
20O, 30O, 60O, 75O, 90O from pole-on view)
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Relevant Spatial Scales

• We need
• Resolution, resolution,
• Spectral resolution
• lt 1 km/s
• Adequate aperture for
• good sensitivity
• Excellent uv-plane
• coverage

(assuming 140 pc)