PowerPoint Presentation - Isolated Neutron Stars, solid crust

Explaining the UV-optical Excess

Turolla, Zane & Drake in preparation

Can we explain the optical excess with a thin, ionized gasoues

layer on the top of the Fe solid?

H deposited by very slow accretion (or fallback). 109g of H in 105 yr Þ deposition rate 10-4 g/s. Orders of magnitude below Bondi.

H is likely not to condensate.

With a typical scale height of 1 cm:

Is ť200 times larger than