000002318 001__ 2318
000002318 005__ 20160701171703.0
000002318 0247_ $$2DOI$$a10.1088/0004-637X/701/1/677
000002318 037__ $$aASTROimport-475
000002318 100__ $$aShaw, G.
000002318 245__ $$aRotationally Warm Molecular Hydrogen in the Orion Bar
000002318 260__ $$c2009
000002318 520__ $$aThe Orion Bar is one of the nearest and best-studied photodissociation or photon-dominated regions (PDRs). Observations reveal the presence of H2 lines from vibrationally or rotationally excited upper levels that suggest warm gas temperatures (400-700 K). However, standard models of PDRs are unable to reproduce such warm rotational temperatures. In this paper, we attempt to explain these observations with new comprehensive models which extend from the H+ region through the Bar and include the magnetic field in the equation of state. We adopt the model parameters from our previous paper which successfully reproduced a wide variety of spectral observations across the Bar. In this model, the local cosmic ray density is enhanced above the galactic background, as is the magnetic field, and which increases the cosmic ray heating elevating the temperature in the molecular region. The pressure is further enhanced above the gas pressure in the H+ region by the momentum transferred from the absorbed starlight. Here, we investigate whether the observed H2 lines can be reproduced with standard assumptions concerning the grain photoelectric emission. We also explore the effects due to the inclusion of recently computed H2 + H2, H2 + H, and H2 + He collisional rate coefficients. 
000002318 700__ $$a Ferland, G. J.
000002318 700__ $$a Henney, W. J.
000002318 700__ $$a Stancil, P. C.
000002318 700__ $$a Abel, N. P.
000002318 700__ $$a Pellegrini, E. W.
000002318 700__ $$a Baldwin, J. A.
000002318 700__ $$a van Hoof, P. A. M.
000002318 773__ $$c677-685$$i1$$pThe Astrophysical Journal$$v701$$y2009
000002318 85642 $$ahttp://esoads.eso.org/abs/2009ApJ...701..677S
000002318 905__ $$apublished in
000002318 980__ $$aREFERD