Carbon-grain Sublimation: A New Top-down Component of Protostellar Chemistry
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Carbon-grain Sublimation : A New Top-down Component of Protostellar Chemistry. / van 't Hoff, Merel L. R.; Bergin, Edwin A.; Jorgensen, Jes K.; Blake, Geoffrey A.
In: Astrophysical Journal Letters, Vol. 897, No. 2, L38, 01.07.2020.Research output: Contribution to journal › Letter › Research › peer-review
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TY - JOUR
T1 - Carbon-grain Sublimation
T2 - A New Top-down Component of Protostellar Chemistry
AU - van 't Hoff, Merel L. R.
AU - Bergin, Edwin A.
AU - Jorgensen, Jes K.
AU - Blake, Geoffrey A.
PY - 2020/7/1
Y1 - 2020/7/1
N2 - Earth's carbon deficit has been an persistent problem in our understanding of the formation of our solar system. A possible solution would be the sublimation of carbon grains at the so-called soot line (similar to 300 K) early in the planet-formation process. Here, we argue that the most likely signatures of this process are an excess of hydrocarbons and nitriles inside the soot line, and a higher excitation temperature for these molecules compared to oxygen-bearing complex organics that desorb around the water snowline (similar to 100 K). Such characteristics have been reported in the literature, for example, in Orion KL, although not uniformly, potentially due to differences in the observational settings and analysis methods of different studies or the episodic nature of protostellar accretion. If this process is active, this would mean that there is a heretofore unknown component to the carbon chemistry during the protostellar phase that is acting from the top down-starting from the destruction of larger species-instead of from the bottom up from atoms. In the presence of such a top-down component, the origin of organic molecules needs to be re-explored.
AB - Earth's carbon deficit has been an persistent problem in our understanding of the formation of our solar system. A possible solution would be the sublimation of carbon grains at the so-called soot line (similar to 300 K) early in the planet-formation process. Here, we argue that the most likely signatures of this process are an excess of hydrocarbons and nitriles inside the soot line, and a higher excitation temperature for these molecules compared to oxygen-bearing complex organics that desorb around the water snowline (similar to 100 K). Such characteristics have been reported in the literature, for example, in Orion KL, although not uniformly, potentially due to differences in the observational settings and analysis methods of different studies or the episodic nature of protostellar accretion. If this process is active, this would mean that there is a heretofore unknown component to the carbon chemistry during the protostellar phase that is acting from the top down-starting from the destruction of larger species-instead of from the bottom up from atoms. In the presence of such a top-down component, the origin of organic molecules needs to be re-explored.
KW - Astrochemistry
KW - Protostars
KW - SPECTRAL-LINE SURVEY
KW - STAR-FORMING REGION
KW - POLYCYCLIC AROMATIC-HYDROCARBONS
KW - COMPLEX ORGANIC-MOLECULES
KW - HOT-CORE
KW - ORION-KL
KW - CHEMICAL DIFFERENTIATION
KW - SURFACE-CHEMISTRY
KW - GHZ
KW - ABUNDANCES
U2 - 10.3847/2041-8213/ab9f97
DO - 10.3847/2041-8213/ab9f97
M3 - Letter
VL - 897
JO - The Astrophysical Journal Letters
JF - The Astrophysical Journal Letters
SN - 2041-8205
IS - 2
M1 - L38
ER -
ID: 246783099