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Radiative Feedback in the Cluster Environment

Setup

• 1000 M SUN clump

• r -‐3/2 density profile

• Axisymmetric, with

rotation

• One of two protostellar

models:

• Peters et al. (2010a)

• Offner et al. (2009)

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HII Region Confined to Protostellar Outflow Figure 3 from Tan & McKee (2003), IAU Symposium 221, Star Formation at High Angular Resolution

Radiative Feedback in the Cluster Environment Setup • 1000 M SUN clump • r -‐3/2 density profile • Axisymmetric, with rotation • One of two protostellar models: • Peters et al. (2010a) • Offner et al. (2009)

Page 1 and 2: Origins of Stars and their Pla
Page 3 and 4: Massive stars are the “movers
Page 5 and 6: Simulating star formation on an
Page 7 and 8: Protostellar Model based on Off
Page 9: Figure 1 from Klassen et al.
Page 13 and 14: Mass-‐Radius Relation for a
Page 15: Column Density (g/cm 2 )
Page 18 and 19: Thank You Ralph Pudritz Thomas
Page 20 and 21: Figure 2 from Klassen et al.
Page 22: Figure 4 from Klassen et al.

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