text: 393,38,1519685299399450629,1074795788331569152,Hayley Beltz,"Just in time for #Exo4, it's new paper day! If you've ever thought to yourself, ""Gee, I wonder what the high resolution emission spectra of an ultrahot Jupiter looks like"" you're in luck! <LINK> First, some background: ultrahot Jupiters (UHJs) have HUGE day-night temperature gradients meaning that we expect their spectra to vary strongly throughout the planet's orbit. (For more info about their atmospheric structure, see my last paper!) <LINK> In fact, depending on the phase, the spectra will show emission features, absorption features, or both. (3D effects!) Check out this little movie showing how the spectra changes as different parts of the planet come into view: <LINK> We also explored the effects of our different magnetic drag treatments. When we look at the net Doppler shifts as a function of phase, we see that on the nightside our dragged models return slight net redshifts compared to the blueshifts seen in the drag-free model. Now the exact values of the shifts are wavelength dependent, but this shows that our differences in the atmospheric structure of magnetic models can show up (and potentially be detected) in high resolution emission spectra. Finally, we end the paper with a warning to those who want to use a single 1D model for their entire observation. Especially near the quadratures, where both day and nightsides are present, a dayside model can retrieve Doppler shifts many km/s away from the true value. Anyways, I hope you check out the paper and I am more than happy to chat about it with anyone interested! @brettmor Thank you!! @_astronomay Thank you!!!!",https://arxiv.org/abs/2204.12996,"Ultrahot Jupiters are ideal candidates to explore with high-resolution emission spectra. Detailed theoretical studies are necessary to investigate the range of spectra we can expect to see from these objects throughout their orbit, because of the extreme temperature and chemical longitudinal gradients that exist across day and nightside regions. Using previously published 3D GCM models of WASP-76b with different treatments of magnetic drag, we post-process the 3D atmospheres to generate high-resolution emission spectra for two wavelength ranges and throughout the planet's orbit. We find that the high-resolution emission spectra vary strongly as a function of phase, at times showing emission features, absorption features, or both, which are a direct result of the 3D structure of the planet. At phases exhibiting both emission and absorption features, the Doppler shift differs in direction between the two spectral features, making them differentiable instead of canceling each other out. Through the use of cross-correlation, we find different patterns in net Doppler shift for models with different treatments of drag: the nightside spectra show opposite signs in their Doppler shift, while the dayside phases have a reversal in the trend of net shift with phase. Finally, we caution researchers from using a single spectral template throughout the planet's orbit; this can bias the corresponding net Doppler shift returned, as it can pick up on a bright region on the edge of the planet disk that is highly red- or blue-shifted. ","Magnetic Drag and 3-D Effects in Theoretical High-Resolution Emission