Scholarlink

<p>The energy deposition of fast electrons in interstellar molecular gas is considered. We use the rotationally resolved cross sections for electron-impact excitation of H<sub>2</sub> molecule that were calculated using the adiabatic-nuclei molecular convergent close-coupling method. The initial electron energy distribution is assumed mono-energetic, and the differential equation for electron energy distribution is solved. We compare calculated energy deposition parameters with the results of similar studies in which the Monte Carlo approach was used. It is shown that about 11 per cent of the initial energy of fast electrons goes into direct ro-vibrational excitation of energy levels of H<sub>2</sub> molecule including pure rotational excitation in neutral molecular gas. About 7 per cent of initial electron energy goes into the excitation to <InlineEquation ID="IEq1"> <EquationSource Format="MATHML"><math> <mi>v</mi> <mo>=</mo> <mn>1</mn> </math></EquationSource> <EquationSource Format="TEX">$v=1$</EquationSource> </InlineEquation> vibrational state of H<sub>2</sub> molecule, most of this energy eventually converts into emission of transitions at near-infrared wavelengths. For ro-vibrational levels with <InlineEquation ID="IEq2"> <EquationSource Format="MATHML"><math> <mi>v</mi> <mo>≥</mo> <mn>3</mn> </math></EquationSource> <EquationSource Format="TEX">$v \geq 3$</EquationSource> </InlineEquation>, the electron-impact excitation to electronic states followed by downward radiative transitions to the ground electronic state is the dominant mechanism of excitation. The yields for excitation to vibrational states via radiative cascading from excited electronic states are found to be <InlineEquation ID="IEq3"> <EquationSource Format="MATHML"><math> <mn>1.5</mn> <mo>−</mo> <mn>2</mn> </math></EquationSource> <EquationSource Format="TEX">$1.5-2$</EquationSource> </InlineEquation> times higher than were obtained in previous studies.</p>

错误：搜索内容不能为空，请输入英文关键词
错误：关键词超出字数限制，请精简
高级检索

Numerical model of fast electron energy deposition in interstellar molecular gas

  • 期刊论文

  • 发表日期：

    2026年6月26日

查看全文
  • Aleksandr Nesterenok

摘要

The energy deposition of fast electrons in interstellar molecular gas is considered. We use the rotationally resolved cross sections for electron-impact excitation of H2 molecule that were calculated using the adiabatic-nuclei molecular convergent close-coupling method. The initial electron energy distribution is assumed mono-energetic, and the differential equation for electron energy distribution is solved. We compare calculated energy deposition parameters with the results of similar studies in which the Monte Carlo approach was used. It is shown that about 11 per cent of the initial energy of fast electrons goes into direct ro-vibrational excitation of energy levels of H2 molecule including pure rotational excitation in neutral molecular gas. About 7 per cent of initial electron energy goes into the excitation to v = 1 $v=1$ vibrational state of H2 molecule, most of this energy eventually converts into emission of transitions at near-infrared wavelengths. For ro-vibrational levels with v ≥ 3 $v \geq 3$ , the electron-impact excitation to electronic states followed by downward radiative transitions to the ground electronic state is the dominant mechanism of excitation. The yields for excitation to vibrational states via radiative cascading from excited electronic states are found to be 1.5 − 2 $1.5-2$ times higher than were obtained in previous studies.