Origin of the unusually low nitrogen abundances in young populations of the Large Magellanic Cloud
Kenji Bekki, Takuji Tsujimoto

TL;DR
The paper investigates the unusually low nitrogen abundances in young populations of the Large Magellanic Cloud, proposing that gas transfer from the Small Magellanic Cloud better explains observations than accretion of low-NH high velocity clouds.
Contribution
It introduces a new scenario attributing low nitrogen abundances to gas transfer from the SMC, challenging the HVC accretion hypothesis for the LMC.
Findings
HVC accretion rates are insufficient to explain low nitrogen levels
Gas transfer from the SMC is a plausible explanation for low [N/H]
Low nitrogen abundances are limited to very young stars (<10^7 yr)
Abstract
It is a longstanding problem that HII regions and very young stellar populations in the Large Magellanic Cloud (LMC) have the nitrogen abundances ([N/H]) by a factor of ~7 lower than the solar value. We here discuss a new scenario in which the observed unusually low nitrogen abundances can be closely associated with recent collision and subsequent accretion of HI high velocity clouds (HVCs) that surround the Galaxy and have low nitrogen abundances. We show that if the observed low [N/H] is limited to very young stars with ages less than ~10^7 yr, then the collision/accretion rate of the HVCs onto the LMC needs to be ~ 0.2 M_sun/yr (corresponding to the total HVC mass of 10^6-10^7 M_sun) to dilute the original interstellar medium (ISM) before star formation. The required accretion rate means that even if the typical mass of HVCs accreted onto the LMC is ~ 10^7 M_sun, the Galaxy needs…
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