We calculate particle spectra and continuum photon emission from the
Cassiopeia A supernova remnant (SNR). The particle spectra, ion and electron,
result from diffusive shock acceleration at the ...forward SNR shock and are
determined with a nonlinear Monte Carlo calculation. The calculation
self-consistently determines the shock structure under the influence of ion
pressure, and includes a simple parameterized treatment of electron injection
and acceleration. Our results are compared to photon observations,
concentrating on the connection between the Radio and GeV-TeV gamma-ray range,
and to cosmic ray ion observations. We include new upper limits from the
Cherenkov Array at Themis (CAT) imaging Cherenkov telescope and the Whipple 10m
gamma-ray telescope at > 400 GeV. These new limits support the suggestion (e.g.
Cowsik & Sarkar 1980; Allen et. al. 1997) that energetic electrons are emitting
synchrotron radiation in an extremely high magnetic field (~ 1000 microGauss),
far greater than values routinely assigned to the ISM, and help to constrain
our model. The large magnetic field allows acceleration of cosmic ray ions to
well above $10^{15}$ eV per nucleon in the ~ 300 yr lifetime of Cas A.
The MRS mode of the JWST-MIRI instrument has been shown to be a powerful tool to characterise the molecular gas emission of the inner region of planet-forming disks. Here, we analyse the spectrum of ...the compact T-Tauri disk DR Tau, which is complemented by high spectral resolution (R~60000-90000) CO ro-vibrational observations. Various molecular species, including CO, CO\(_2\), HCN, and C\(_2\)H\(_2\) are detected in the JWST-MIRI spectrum, for which excitation temperatures of T~325-900 K are retrieved using LTE slab models. The high-resolution CO observations allow for a full treatment of the line profiles, which show evidence for two components of the main isotopologue, \(^{12}\)CO: a broad component tracing the Keplerian disk and a narrow component tracing a slow disk wind. Rotational diagrams yield excitation temperatures of T>725 K for CO, with consistently lower temperatures found for the narrow components, suggesting that the disk wind is launched from a larger distance. The inferred excitation temperatures for all molecules suggest that CO originates from the highest atmospheric layers close to the host star, followed by HCN and C\(_2\)H\(_2\), which emit, together with \(^{13}\)CO, from slightly deeper layers, whereas the CO\(_2\) originates from even deeper inside or further out in the disk. Additional analysis of the \(^{12}\)CO line wings hint at a misalignment between the inner (i~20 degrees) and outer disk (i~5 degrees). Finally, we emphasise the need for complementary high-resolution CO observations, as in combination with the JWST-MIRI observations they can be used to characterise the CO kinematics and the physical and chemical conditions of the other observed molecules with respect to CO.
