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Resolved Inner Disks around Herbig Ae/Be Stars:
Near-IR Interferometry with PTIJosh Eisner
Collaborators: Ben Lane, Lynne Hillenbrand, Rachel Akeson, and Anneila Sargent
• Eisner et al. 2003, ApJ, 598, 1341• Eisner et al. 2004, ApJ, submitted
Ringberg Castle, 2004
Circumstellar Disks
• Disks linked to star and planet-formation
• Accretion mechanism: IMF, stellar rotation, magnetic properties, outflows
• Disk properties (e.g., temperature, density, geometry) dictate planetary properties
• Relation to proto-solar nebula
Artist’s conception of TW Hya Disk
• Herbig Ae/Be stars:– Higher-mass analog of T Tauris: 2-10 M
– Emission lines,variability, excess IR and mm emission
• SED models: thin accretion disks (Hillenbrand et al. 1992), flared disks (Chiang & Goldreich 1997), puffed up inner disk walls (Dullemond et al. 2001)
• Forbidden emission lines (Corcoran & Ray 1997)• H spectropolarimetry (Vink et al. 2002)• Resolved mm emission: flattened structures on
100 AU scales with Keplerian rotation• Strong evidence from new near-IR interferometry
(Corcoran & Ray 1997)
• Herbig Ae/Be stars:– Higher-mass analog of T Tauris: 2-10 M
– Emission lines,variability, excess IR and mm emission
• SED models: thin accretion disks (Hillenbrand et al. 1992), flared disks (Chiang & Goldreich 1997), puffed up inner disk walls (Dullemond et al. 2001)
• Forbidden emission lines (Corcoran & Ray 1997)• H spectropolarimetry (Vink et al. 2002)• Resolved mm emission: flattened structures on
100 AU scales with Keplerian rotation• Strong evidence from new near-IR interferometry
(Dullemond, Dominik, & Natta 2001)
• Herbig Ae/Be stars:– Higher-mass analog of T Tauris: 2-10 M
– Emission lines,variability, excess IR and mm emission
• SED models: thin accretion disks (Hillenbrand et al. 1992), flared disks (Chiang & Goldreich 1997), puffed up inner disk walls (Dullemond et al. 2001)
• Forbidden emission lines (Corcoran & Ray 1997)• H spectropolarimetry (Vink et al. 2002)• Resolved mm emission: flattened structures on
100 AU scales with Keplerian rotation• Strong evidence from new near-IR interferometry
Disks Around HAEBEs
(Vink et al. 2002)
• Herbig Ae/Be stars:– Higher-mass analog of T Tauris: 2-10 M
– Emission lines,variability, excess IR and mm emission
• SED models: thin accretion disks (Hillenbrand et al. 1992), flared disks (Chiang & Goldreich 1997), puffed up inner disk walls (Dullemond et al. 2001)
• Forbidden emission lines (Corcoran & Ray 1997)• H spectropolarimetry (Vink et al. 2002)• Resolved mm emission: flattened structures on
100 AU scales with Keplerian rotation• Strong evidence from new near-IR interferometry
(Mannings & Sargent 1997)
• Herbig Ae/Be stars:– Higher-mass analog of T Tauris: 2-10 M
– Emission lines,variability, excess IR and mm emission
• SED models: thin accretion disks (Hillenbrand et al. 1992), flared disks (Chiang & Goldreich 1997), puffed up inner disk walls (Dullemond et al. 2001)
• Forbidden emission lines (Corcoran & Ray 1997)• H spectropolarimetry (Vink et al. 2002)• Resolved mm emission: flattened structures on
100 AU scales with Keplerian rotation• Strong evidence from new near-IR interferometry
< 0.1-1 AU
• Herbig Ae/Be stars:– Higher-mass analog of T Tauris: 2-10 M
– Emission lines,variability, excess IR and mm emission
• SED models: thin accretion disks (Hillenbrand et al. 1992), flared disks (Chiang & Goldreich 1997), puffed up inner disk walls (Dullemond et al. 2001)
• Forbidden emission lines (Corcoran & Ray 1997)• H spectropolarimetry (Vink et al. 2002)• Resolved mm emission: flattened structures on
100 AU scales with Keplerian rotation• Strong evidence from new near-IR interferometry
…
Palomar Testbed Interferometer
(PTI)
• PTI observations allow large sample, good uv coverage
• longer baselines facilitate detection of asymmetry
• PTI components: – 3 telescopes each 0.4 m
• 110 m NS oriented 20º E of N (4 mas)• 85 m NW oriented 81º E of N (5 mas)• 87 m SW baseline recently operational!
• No significant mis-alignment of inner and outer disks
• Different vertical disk structure for early and late spectral types– Flat accretion disks better for early-types– Flared disks w/ puffed-up inner walls for later types– Magnetospheric accretion in HAes vs. Equatorial