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Modeling Surface Brightness of the HH 901 Jets in the Carina Nebula

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The purpose of this thesis is to accurately simulate the surface brightness in various spectral emission lines of the HH 901 jets in the Mystic Mountain Formation of the Carina Nebula. To accomplish this goal, we gathered relevant spectral emission

The purpose of this thesis is to accurately simulate the surface brightness in various spectral emission lines of the HH 901 jets in the Mystic Mountain Formation of the Carina Nebula. To accomplish this goal, we gathered relevant spectral emission line data for [Fe II] 12660 Å, Hα 6563 Å, and [S II] 6720 Å to compare with Hubble Space Telescope observations of the HH 901 jets presented in Reiter et al. (2016). We derived the emissivities for these lines from the spectral synthesis code Cloudy by Ferland et al. (2017). In addition, we used WENO simulations of density, temperature, and radiative cooling to model the jet. We found that the computed surface brightness values agreed with most of the observational surface brightness values. Thus, the 3D cylindrically symmetric simulations of surface brightness using the WENO code and Cloudy spectral emission models are accurate for jets like HH 901. After detailing these agreements, we discuss the next steps for the project, like adding an external ambient wind and performing the simulations in full 3D.

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Date Created
2020-05

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Numerical Simulation of the Carina Nebula Astrophysical Jets

Description

This project attempts to create an accurate numerical simulation of the eastern limb of the HH 901 jet in the Mystic Mountain formation located in the Carina Nebula. Using a 3rd order accurate WENO numerical scheme in space, and a

This project attempts to create an accurate numerical simulation of the eastern limb of the HH 901 jet in the Mystic Mountain formation located in the Carina Nebula. Using a 3rd order accurate WENO numerical scheme in space, and a 3rd order accurate RK method in time, the temperature, density, radiative cooling, length, and average jet velocity of this astrophysical phenomenon were simulated based on observations made by Hubble Space Telescope and the work of Reiter and Smith (2013) and (2014). The results of this simulation are displayed in three figures, one each for temperature, radiative cooling, and density, which show a jet displaying morphology consistent with that of the HH 901 eastern limb without adjustment for stellar wind. Also discussed are the effects of different jet speeds, initial conditions, and pulse parameters on the shape and behavior of the simulated jets, as well as continuing work to be done on the simulation to enhance its accuracy and usefulness.

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Date Created
2019-05