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Suppression of star formation in dwarf galaxies by photoelectric grain heating feedback

机译：光电粒子加热反馈对矮星系恒星形成的抑制

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Photoelectric heating-heating of dust grains by far-ultraviolet photons-has long been recognized as the primary source of heating for the neutral interstellar medium(1). Simulations of spiral galaxies(2) have shown some indication that photoelectric heating could suppress star formation; however, simulations that include photoelectric heating have typically shown that it has little effect on the rate of star formation in either spiral galaxies(3,4) or dwarf galaxies(5), which suggests that supernovae are responsible for setting the gas depletion time in galaxies(6-8). This result is in contrast with recent work(9-13) indicating that a star formation law that depends on galaxy metallicity-as is expected with photoelectric heating, but not with supernovae-reproduces the present-day galaxy population better than does a metallicity-independent one. Here we report a series of simulations of dwarf galaxies, the class of galaxy in which the effects of both photoelectric heating and supernovae are expected to be strongest. We simultaneously include space-and time-dependent photoelectric heating in our simulations, and we resolve the energy-conserving phase of every supernova blast wave, which allows us to directly measure the relative importance of feedback by supernovae and photoelectric heating in suppressing star formation. We find that supernovae are unable to account for the observed(14) large gas depletion times in dwarf galaxies. Instead, photoelectric heating is the dominant means by which dwarf galaxies regulate their star formation rate at any given time, suppressing the rate by more than an order of magnitude relative to simulations with only supernovae.
机译：长期以来，人们一直认为光电加热-利用远紫外光子加热尘埃颗粒是中性星际介质的主要加热源（1）。旋涡星系的模拟（2）表明，光电加热可以抑制恒星的形成。但是，包括光电加热的模拟通常显示，它对旋涡星系（3,4）或矮星系（5）中恒星形成的速率几乎没有影响，这表明超新星是决定恒星中气体耗尽时间的原因。星系（6-8）。这个结果与最近的研究（9-13）相反，后者表明取决于银河金属性的恒星形成定律（如光电加热所期望的那样，而不是超新星）则比金属性更好地再现了当今的银河系。独立的。在这里，我们报告一系列矮星系的模拟，矮星系是其中光电加热和超新星效应都预计最强的银河系。我们在模拟中同时包括了时空依赖的光电加热，并且解析了每个超新星爆炸波的能量守恒阶段，这使我们能够直接测量超新星和光电加热反馈在抑制恒星形成方面的相对重要性。我们发现，超新星无法解释矮星系中观测到的（14）大气体耗竭时间。取而代之的是，光电加热是矮星系在任何给定时间调节其恒星形成速率的主要手段，相对于仅具有超新星的模拟，该速率将速率抑制了一个数量级以上。

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  • 来源
    《Nature》 |2016年第7613期|523-525|共3页
  • 作者

    Forbes John C.; Krumholz Mark R.; Goldbaum Nathan J.; Dekel Avishai;

  • 作者单位

    Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA;

    Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA|Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia;

    Univ Illinois, Natl Ctr Supercomp Applicat, 1205 West Clark St, Urbana, IL 61820 USA;

    Hebrew Univ Jerusalem, Racah Inst Phys, Ctr Astrophys & Planetary Sci, IL-91904 Jerusalem, Israel;

  • 收录信息 美国《科学引文索引》(SCI);美国《工程索引》(EI);美国《生物学医学文摘》(MEDLINE);美国《化学文摘》(CA);
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