title: Ð­ÑÑÐµÐºÑÑ Ð¿ÐµÑÐµÐ½Ð¾ÑÐ° Ð¸Ð·Ð»ÑÑÐµÐ½Ð¸Ñ Ð² Ð»Ð¸Ð½Ð¸ÑÑ HeI, Ð¾Ð±ÑÐ°Ð·ÑÑÑÐ¸Ñ ÑÑ Ð² Ð¸Ð¾Ð½Ð¸Ð·Ð¸ÑÐ¾Ð²Ð°Ð½Ð½Ð¾Ð¹ Ð¼ÐµÐ¶Ð·Ð²ÐµÐ·Ð´Ð½Ð¾Ð¹ ÑÑÐµÐ´Ðµ
title: Ð²ÑÐ¿ÑÑÐºÐ½Ð°Ñ ÐºÐ²Ð°Ð»Ð¸ÑÐ¸ÐºÐ°ÑÐ¸Ð¾Ð½Ð½Ð°Ñ ÑÐ°Ð±Ð¾ÑÐ° Ð±Ð°ÐºÐ°Ð»Ð°Ð²ÑÐ°
titleType: Subtitle
title: Effects of radiation transfer in HeI lines formed in an ionized interstellar medium
Creators: name: ÐÐ¾Ð·Ð»Ð¾Ð²ÑÐºÐ°Ñ, ÐÐ½Ð½Ð°
Publisher: name: Ð¡Ð°Ð½ÐºÑ-ÐÐµÑÐµÑÐ±ÑÑÐ³ÑÐºÐ¸Ð¹ Ð¿Ð¾Ð»Ð¸ÑÐµÑÐ½Ð¸ÑÐµÑÐºÐ¸Ð¹ ÑÐ½Ð¸Ð²ÐµÑÑÐ¸ÑÐµÑ ÐÐµÑÑÐ° ÐÐµÐ»Ð¸ÐºÐ¾Ð³Ð¾
Year: 2024
Subjects: ÑÑÐ½ÐºÑÐ¸Ñ Ð¾Ð¿ÑÐ¸ÑÐµÑÐºÐ¾Ð¹ ÑÐ¾Ð»ÑÐ¸
ÑÐ¼Ð¸ÑÑÐ¸Ð¾Ð½Ð½ÑÐµ Ð»Ð¸Ð½Ð¸Ð¸ Ð³ÐµÐ»Ð¸Ñ
Ð¿ÐµÑÐ²Ð¸ÑÐ½ÑÐ¹ Ð½ÑÐºÐ»ÐµÐ¾ÑÐ¸Ð½ÑÐµÐ·
Ð¾Ð¿ÑÐ¸ÑÐµÑÐºÐ°Ñ ÑÐ¾Ð»ÑÐ°
Ð¸ÑÐ¿ÑÑÐºÐ°ÑÐµÐ»ÑÐ½ÑÐµ ÑÐ¿Ð¾ÑÐ¾Ð±Ð½Ð¾ÑÑÐ¸ Ð»Ð¸Ð½Ð¸Ð¹
ÑÑÐ¸Ð¿Ð»ÐµÑÐ½ÑÐµ Ð¸ ÑÐ¸Ð½Ð³Ð»ÐµÑÐ½ÑÐµ ÑÐ¾ÑÑÐ¾ÑÐ½Ð¸Ñ
Ð³ÐµÐ»Ð¸Ð¹
Ð·Ð°ÑÐµÐ»ÐµÐ½Ð½Ð¾ÑÑÐ¸ ÑÐ½ÐµÑÐ³ÐµÑÐ¸ÑÐµÑÐºÐ¸Ñ ÑÑÐ¾Ð²Ð½ÐµÐ¹
ÑÑÐ°Ð²Ð½ÐµÐ½Ð¸Ðµ Ð´ÐµÑÐ°Ð»ÑÐ½Ð¾Ð³Ð¾ Ð±Ð°Ð»Ð°Ð½ÑÐ°
ÑÐµÑÐµÐ½Ð¸Ñ Ð¸Ð¾Ð½Ð¸Ð·Ð°ÑÐ¸Ð¸
ÑÐµÑÐµÐ½Ð¸Ñ ÑÐµÐºÐ¾Ð¼Ð±Ð¸Ð½Ð°ÑÐ¸Ð¸
optical depth function
helium emission lines
primary nucleosynthesis
optical depth
line emissivity
triplet and singlet states
helium
population of energy levels
equation of statistical equilibrium
ionization cross sections
recombination cross sections

description: ÐÐ°Ð½Ð½Ð°Ñ ÑÐ°Ð±Ð¾ÑÐ° Ð¿Ð¾ÑÐ²ÑÑÐµÐ½Ð° ÑÑÑÐµÐºÑÐ°Ð¼ Ð¿ÐµÑÐµÐ½Ð¾ÑÐ° Ð¸Ð·Ð»ÑÑÐµÐ½Ð¸Ñ HeI, ÑÐ²ÑÐ·Ð°Ð½Ð½ÑÐ¼ Ñ Ð²Ð»Ð¸ÑÐ½Ð¸ÐµÐ¼ Ð¾Ð¿ÑÐ¸ÑÐµÑÐºÐ¾Ð¹ ÑÐ¾Ð»ÑÐ¸ Ð½Ð° Ð¼ÐµÑÐ°ÑÑÐ°Ð±Ð¸Ð»ÑÐ½Ð¾Ð¼ ÑÑÐ¾Ð²Ð½Ðµ ÑÑÐ¸Ð¿Ð»ÐµÑÐ½Ð¾Ð¹ ÑÐµÑÐ¸Ð¸ Ð½Ð° Ð¸ÑÐ¿ÑÑÐºÐ°ÑÐµÐ»ÑÐ½ÑÑ ÑÐ¿Ð¾ÑÐ¾Ð±Ð½Ð¾ÑÑÑ Ð»Ð¸Ð½Ð¸Ð¹ Ð½ÐµÐ¹ÑÑÐ°Ð»ÑÐ½Ð¾Ð³Ð¾ Ð³ÐµÐ»Ð¸Ñ. Ð ÑÐ¾Ð´Ðµ ÑÐ°Ð±Ð¾ÑÑ Ð±ÑÐ»Ð¾ ÑÐ°ÑÑÐ¼Ð¾ÑÑÐµÐ½Ð¾ Ð¸Ð·Ð¼ÐµÐ½ÐµÐ½Ð¸Ðµ ÑÑÐ½ÐºÑÐ¸Ð¸ Ð¾Ð¿ÑÐ¸ÑÐµÑÐºÐ¾Ð¹ ÑÐ¾Ð»ÑÐ¸ Ð´Ð»Ñ Ð»Ð¸Ð½Ð¸Ð¹ ÑÑÐ¸Ð¿Ð»ÐµÑÐ½Ð¾Ð¹ ÑÐµÑÐ¸Ð¸ Ð¿ÑÐ¸ Ð¸ÑÐ¿Ð¾Ð»ÑÐ·Ð¾Ð²Ð°Ð½Ð¸Ð¸ Ð² ÑÐ°ÑÑÐµÑÐµ Ð±Ð¾Ð»ÐµÐµ Ð°ÐºÑÑÐ°Ð»ÑÐ½ÑÑ Ð°ÑÐ¾Ð¼Ð½ÑÑ Ð´Ð°Ð½Ð½ÑÑ. ÐÐ»Ñ Ð¿Ð¾Ð»ÑÑÐµÐ½Ð¸Ñ ÑÑÐ¾ÑÐ½ÐµÐ½Ð½Ð¾Ð¹ ÑÑÐ½ÐºÑÐ¸Ð¸ Ð¾Ð¿ÑÐ¸ÑÐµÑÐºÐ¾Ð¹ ÑÐ¾Ð»ÑÐ¸ ÑÐ¸ÑÐ»ÐµÐ½Ð½Ð¾ Ð±ÑÐ»Ð¾ ÑÐµÑÐµÐ½Ð¾ ÑÑÐ°Ð²Ð½ÐµÐ½Ð¸Ðµ Ð´ÐµÑÐ°Ð»ÑÐ½Ð¾Ð³Ð¾ Ð±Ð°Ð»Ð°Ð½ÑÐ° Ð´Ð»Ñ Ð¼Ð¾Ð´ÐµÐ»Ð¸ ÑÐ¾ÑÑÐ¾ÑÑÐµÐ¹ Ð¸Ð· n = 5 ÑÑÐ¾Ð²Ð½ÐµÐ¹. Ð¢Ð°ÐºÐ¶Ðµ Ð±ÑÐ»Ð¸ Ð¸Ð·Ð¼ÐµÐ½ÐµÐ½Ñ Ð°ÑÐ¾Ð¼Ð½ÑÐµ Ð´Ð°Ð½Ð½ÑÐµ Ð´Ð»Ñ ÐºÐ¾ÑÑÑÐ¸ÑÐ¸ÐµÐ½ÑÐ¾Ð² Ð­Ð¹Ð½ÑÑÐµÐ¹Ð½Ð°, ÐºÐ¾ÑÑÑÐ¸ÑÐ¸ÐµÐ½ÑÐ¾Ð² ÑÑÐ¾Ð»ÐºÐ½Ð¾Ð²Ð¸ÑÐµÐ»ÑÐ½Ð¾Ð¹ Ð¸Ð¾Ð½Ð¸Ð·Ð°ÑÐ¸Ð¸, ÐºÐ¾ÑÑÑÐ¸ÑÐ¸ÐµÐ½ÑÐ¾Ð² ÑÑÐ¾Ð»ÐºÐ½Ð¾Ð²Ð¸ÑÐµÐ»ÑÐ½Ð¾Ð³Ð¾ Ð²Ð¾Ð·Ð±ÑÐ¶Ð´ÐµÐ½Ð¸Ñ Ð¸ ÑÐµÐºÐ¾Ð¼Ð±Ð¸Ð½Ð°ÑÐ¸Ð¸ Ð¸ ÐºÐ¾ÑÑÑÐ¸ÑÐ¸ÐµÐ½ÑÐ¾Ð² ÑÑÐµÑÑÐ°ÑÑÐ¸ÑÐ½Ð¾Ð¹ ÑÐµÐºÐ¾Ð¼Ð±Ð¸Ð½Ð°ÑÐ¸Ð¸. ÐÑÐ»Ð¾ Ð¿Ð¾ÐºÐ°Ð·Ð°Ð½Ð¾, ÑÑÐ¾ Ð½Ð°Ð¸Ð±Ð¾Ð»ÑÑÐ¸Ð¹ Ð²ÐºÐ»Ð°Ð´ Ð² Ð¸Ð·Ð¼ÐµÐ½ÐµÐ½Ð¸Ðµ ÑÐµÐ·ÑÐ»ÑÑÐ¸ÑÑÑÑÐµÐ¹ ÑÑÐ½ÐºÑÐ¸Ð¸ Ð²Ð½Ð¾ÑÑÑ ÐºÐ¾ÑÑÑÐ¸ÑÐ¸ÐµÐ½ÑÑ ÑÑÐ¾Ð»ÐºÐ½Ð¾Ð²Ð¸ÑÐµÐ»ÑÐ½Ð¾Ð¹ Ð¸Ð¾Ð½Ð¸Ð·Ð°ÑÐ¸Ð¸, Ð° ÑÐ°ÐºÐ¶Ðµ ÐºÐ¾ÑÑÑÐ¸ÑÐ¸ÐµÐ½ÑÑ ÑÑÐ¾Ð»ÐºÐ½Ð¾Ð²Ð¸ÑÐµÐ»ÑÐ½Ð¾Ð³Ð¾ Ð²Ð¾Ð·Ð±ÑÐ¶Ð´ÐµÐ½Ð¸Ñ Ð¸ ÑÐµÐºÐ¾Ð¼Ð±Ð¸Ð½Ð°ÑÐ¸Ð¸. ÐÐ°Ð¸Ð±Ð¾Ð»ÐµÐµ ÑÐ¸Ð»ÑÐ½Ð¾ Ð¸Ð·Ð¼ÐµÐ½ÐµÐ½Ð¸Ñ Ð¾ÐºÐ°Ð·Ð°Ð»Ð°ÑÑ Ð¿Ð¾Ð´Ð²ÐµÑÐ¶ÐµÐ½Ð° Ð»Ð¸Ð½Ð¸Ñ Î» = 7065ËA, Ð½Ð°Ð¸Ð¼ÐµÐ½ÑÑÐ¸Ðµ Ð¸Ð·Ð¼ÐµÐ½ÐµÐ½Ð¸Ñ Ð±ÑÐ»Ð¸ Ð·Ð°Ð¼ÐµÑÐµÐ½Ñ Ð² ÑÑÐ½ÐºÑÐ¸Ð¸ Ð¾Ð¿ÑÐ¸ÑÐµÐºÐ¾Ð¹ ÑÐ¾Ð»ÑÐ¸ Ð´Ð»Ñ Ð»Ð¸Ð½Ð¸Ð¹ Î» = 2945ËA Ð¸ Î» = 3189ËA. ÐÐ°Ð½Ð½Ð°Ñ ÑÐ°Ð±Ð¾ÑÐ° ÑÐ²Ð»ÑÐµÑÑÑ ÑÐ°ÑÑÑÑ Ð³ÐµÐ»Ð¸ÐµÐ²Ð¾Ð¹ Ð¿ÑÐ¾Ð±Ð»ÐµÐ¼Ñ Ð¸ Ð¼Ð¾Ð¶ÐµÑ Ð±ÑÑÑ Ð¿ÑÐ¾Ð´Ð¾Ð»Ð¶ÐµÐ½Ð° Ð²ÑÑÐ¸ÑÐ»ÐµÐ½Ð¸ÐµÐ¼ ÑÐ¾Ð´ÐµÑÐ¶Ð°Ð½Ð¸Ñ Ð¿ÐµÑÐ²Ð¸ÑÐ½Ð¾Ð³Ð¾ Ð³ÐµÐ»Ð¸Ñ.
description: The given work is devoted to the effects of radiation transfer HeI associated with the influence of the optical depth at the metastable level of the triplet series on the emissivity of neutral helium lines. in the process of work, the change in the optical depth function for triplet series lines was considered when using up-to-date atomic data in the calculation. To obtain a refined function of the optical depth, the detailed balance equation for the model consisting of n = 5 levels was numerically solved. The atomic data for Einstein coefficients, collisional ionization coefficients, collisional excitation and recombination coefficients, and three-particle recombination coefficients were also changed. It was shown that the greatest contribution to the change in the resulting function is made by the coefficients of collisional ionization, as well as the coefficients of collisional excitation and recombination. The line Î» = 7065ËA was most strongly affected, the smallest changes were observed in the optical thickness function for the lines Î» = 2945ËA and Î» = 3189ËA. This work is part of the helium problem and can be continued by calculating the primary helium abundance.