Acetonitrile Photochemistry in Interstellar Ice Analogs

Authors:

Selina Hokello, Michelle Brann, Karin berg

Date Created:

2025-01-01

Course Title:

Professor:

Not specified

About Paper:

▯19 2 ▯1 Nitriles, including acetonitrile (3H CN), have been detected in the7:54 ▯ 10 cm photon . For CH C3:CO ices (ratios icy grain mantles within the protoplanetary disk of stars. The disk2.5:1 to 1:18) and CH C3:H O i2es (ratios 1:9 to 1:11) at 15K, of star MWC 480 has been observed to resemble the foundational the destruction rates increased by 48% and 172%, respectively, chemistry of our Solar System, so understanding the molecular in comparison to the pure CH CN ice. The survival yield of behavior within these disks can inform us about how planetary CH C3 at 15K was approximately 45% in pure CH CN, 13 %3 systems are formed. We investigate CH C3 UV photodestruction in CH 3N:CO, and 33% in CH CN:H 3. Thes2 findings suggest and how that rate changes based on ice temperature and chemical that the chemical matrix does impact the destruction of CH C3. matrix. An ultra-high vacuum chamber is used to build these ices Additionally, pure CH C3 ices showed a possible influence of with gas mixtures of pure CH C3, CH CN 3n carbon monoxide temperature on destruction, with higher temperatures leading to (CO), and CH C3 in water (H O) 2t temperatures between 15K- a slight increase in the rate and amount destroyed over time. 100K. Upon Python analysis of the IR spectra, we curve-fit the Overall, these findings highlight the importance of the ice matrix normalized data to determine the destruction rate and the amount for the destruction of CH 3N and broaden our understanding of destroyed. Pure CH C3 ices at 15K and approximately 50 ice photochemistry around stars. monolayers had an average destruction rate of 3:72 ▯ 10 ▯18 ▯

Abstract:

▯19 2 ▯1 Nitriles, including acetonitrile (3H CN), have been detected in the7:54 ▯ 10 cm photon . For CH C3:CO ices (ratios icy grain mantles within the protoplanetary disk of stars. The disk2.5:1 to 1:18) and CH C3:H O i2es (ratios 1:9 to 1:11) at 15K, of star MWC 480 has been observed to resemble the foundational the destruction rates increased by 48% and 172%, respectively, chemistry of our Solar System, so understanding the molecular in comparison to the pure CH CN ice. The survival yield of behavior within these disks can inform us about how planetary CH C3 at 15K was approximately 45% in pure CH CN, 13 %3 systems are formed. We investigate CH C3 UV photodestruction in CH 3N:CO, and 33% in CH CN:H 3. Thes2 findings suggest and how that rate changes based on ice temperature and chemical that the chemical matrix does impact the destruction of CH C3. matrix. An ultra-high vacuum chamber is used to build these ices Additionally, pure CH C3 ices showed a possible influence of with gas mixtures of pure CH C3, CH CN 3n carbon monoxide temperature on destruction, with higher temperatures leading to (CO), and CH C3 in water (H O) 2t temperatures between 15K- a slight increase in the rate and amount destroyed over time. 100K. Upon Python analysis of the IR spectra, we curve-fit the Overall, these findings highlight the importance of the ice matrix normalized data to determine the destruction rate and the amount for the destruction of CH 3N and broaden our understanding of destroyed. Pure CH C3 ices at 15K and approximately 50 ice photochemistry around stars. monolayers had an average destruction rate of 3:72 ▯ 10 ▯18 ▯

Source:

Harvard / Harvard College | Lowell House | Chemistry | 2028 / 2025

Topics:

destruction, ice, rate, pure, ices, temperature, star, chemistry, matrix, acetonitrile, photochemistry, ratio

Co-authors:

@selinahokello291 , @michellebrann292 , @karinberg176