On detection of BaO molecular lines in sunspot spectrum

IF 1.9 4区 物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS
P. Sriramachandran , S.H. Nivash
{"title":"On detection of BaO molecular lines in sunspot spectrum","authors":"P. Sriramachandran ,&nbsp;S.H. Nivash","doi":"10.1016/j.ascom.2024.100891","DOIUrl":null,"url":null,"abstract":"<div><h3>Context</h3><div>Spectral lines of diatomic molecules are perfect tools for studying the structure of sunspots and their temperature layers and magnetic sensitive absorption features, which are typically higher than in atomic lines. The integrated intensities of a few bands in the rotational structure of the astrophysically significant <span><math><mrow><msup><mi>A</mi><mn>1</mn></msup><msup><mrow><mstyle><mi>Σ</mi></mstyle></mrow><mo>+</mo></msup><mo>−</mo><msup><mi>X</mi><mn>1</mn></msup><msup><mrow><mstyle><mi>Σ</mi></mstyle></mrow><mo>+</mo></msup></mrow></math></span>and <span><math><mrow><mi>A</mi><msup><mrow></mrow><mrow><mo>′</mo><mn>1</mn></mrow></msup><mstyle><mi>Π</mi></mstyle><mo>−</mo><msup><mi>X</mi><mn>1</mn></msup><msup><mrow><mstyle><mi>Σ</mi></mstyle></mrow><mo>+</mo></msup></mrow></math></span> systems of barium monoxide (BaO) have been measured experimentally using band spectra. An analysis of the prominent lines of (0, 0; 1, 1; 2, 2) bands of <span><math><mrow><msup><mi>A</mi><mn>1</mn></msup><msup><mrow><mstyle><mi>Σ</mi></mstyle></mrow><mo>+</mo></msup><mo>−</mo><msup><mi>X</mi><mn>1</mn></msup><msup><mrow><mstyle><mi>Σ</mi></mstyle></mrow><mo>+</mo></msup></mrow></math></span>transition and (0, 0; 1, 1; 2, 2) bands of <span><math><mrow><mi>A</mi><msup><mrow></mrow><mrow><mo>′</mo><mn>1</mn></mrow></msup><mstyle><mi>Π</mi></mstyle><mo>−</mo><msup><mi>X</mi><mn>1</mn></msup><msup><mrow><mstyle><mi>Σ</mi></mstyle></mrow><mo>+</mo></msup><mspace></mspace></mrow></math></span>transition with those of sunspot umbral spectrum. The effective rotational temperatures of the <span><math><mrow><mi>A</mi><msup><mrow></mrow><mrow><mo>′</mo><mn>1</mn></mrow></msup><mstyle><mi>Π</mi></mstyle><mo>−</mo><msup><mi>X</mi><mn>1</mn></msup><msup><mrow><mstyle><mi>Σ</mi></mstyle></mrow><mo>+</mo></msup><mspace></mspace></mrow></math></span>transition of BaO in the sunspot umbral spectrum are found to be in the range of 1600 K to 3200 K.</div></div><div><h3>Aims</h3><div>An analysis of BaO prominent rotational molecular lines of <span><math><mrow><msup><mi>A</mi><mn>1</mn></msup><msup><mrow><mstyle><mi>Σ</mi></mstyle></mrow><mo>+</mo></msup><mo>−</mo><msup><mi>X</mi><mn>1</mn></msup><msup><mrow><mstyle><mi>Σ</mi></mstyle></mrow><mo>+</mo></msup></mrow></math></span>and <span><math><mrow><mi>A</mi><msup><mrow></mrow><mrow><mo>′</mo><mn>1</mn></mrow></msup><mstyle><mi>Π</mi></mstyle><mo>−</mo><msup><mi>X</mi><mn>1</mn></msup><msup><mrow><mstyle><mi>Σ</mi></mstyle></mrow><mo>+</mo></msup><mspace></mspace></mrow></math></span>transition with those of sunspot umbral spectral lines. To find the significant values of radiative transition parameters, vibrational temperature and the effective rotational temperature of the molecule in celestial objects.</div></div><div><h3>Methods</h3><div>Calibrated the rotational structure of molecular band heads and lines for and <span><math><mrow><msup><mi>A</mi><mn>1</mn></msup><msup><mrow><mstyle><mi>Σ</mi></mstyle></mrow><mo>+</mo></msup><mo>−</mo><msup><mi>X</mi><mn>1</mn></msup><msup><mrow><mstyle><mi>Σ</mi></mstyle></mrow><mo>+</mo></msup></mrow></math></span>and <span><math><mrow><mi>A</mi><msup><mrow></mrow><mrow><mo>′</mo><mn>1</mn></mrow></msup><mstyle><mi>Π</mi></mstyle><mo>−</mo><msup><mi>X</mi><mn>1</mn></msup><msup><mrow><mstyle><mi>Σ</mi></mstyle></mrow><mo>+</mo></msup><mspace></mspace></mrow></math></span>ransitions in laboratory spectrum using most precise Hartmann's technique. High resolution FTS sunspot umbral spectra from NSO/Kitt Peak were used to detect rotational molecular lines due to the <span><math><mrow><mi>A</mi><msup><mrow></mrow><mrow><mo>′</mo><mn>1</mn></mrow></msup><mstyle><mi>Π</mi></mstyle><mo>−</mo><msup><mi>X</mi><mn>1</mn></msup><msup><mrow><mstyle><mi>Σ</mi></mstyle></mrow><mo>+</mo></msup><mspace></mspace></mrow></math></span>transition of the BaO molecule using the method of line coincidence. The effective rotational temperature was derived from the variation of equivalent width <span><math><mrow><mo>(</mo><mi>W</mi><mo>)</mo></mrow></math></span> with rotational quantum number <span><math><mrow><mo>(</mo><mi>J</mi><mo>)</mo></mrow></math></span> of spectrally well resolved rotational lines of a band in umbral spectrum. The triangular profile approximation method was used to estimate the equivalent width of the well resolved spectral lines.</div></div><div><h3>Results</h3><div>The effective rotational temperatures of the <span><math><mrow><mi>A</mi><msup><mrow></mrow><mrow><mo>′</mo><mn>1</mn></mrow></msup><mstyle><mi>Π</mi></mstyle><mo>−</mo><msup><mi>X</mi><mn>1</mn></msup><msup><mrow><mstyle><mi>Σ</mi></mstyle></mrow><mo>+</mo></msup><mspace></mspace></mrow></math></span>transition of BaO in the sunspot umbral spectrum are found to be in the range of 1600 K to 3200 K. It is compared with other results with a view to obtaining useful physical parameters. This is an evidence to ascertain the possible presence of BaO molecule in solar spectrum in different layers.</div></div><div><h3>Conclusions</h3><div>Unblended rotational lines due to the band of BaO, provide a good range of temperatures for the study of absorbing layers in umbral spectra. The <span><math><mrow><mi>A</mi><msup><mrow></mrow><mrow><mo>′</mo><mn>1</mn></mrow></msup><mstyle><mi>Π</mi></mstyle><mo>−</mo><msup><mi>X</mi><mn>1</mn></msup><msup><mrow><mstyle><mi>Σ</mi></mstyle></mrow><mo>+</mo></msup><mspace></mspace></mrow></math></span>transition of BaO molecular lines is found to be very sensitive to effective temperature. Radiative transition parameters data of these lines, in contrast to intensity measurements, provide us with more direct and detailed information to study the coolest parts of sunspot umbrae.</div></div>","PeriodicalId":48757,"journal":{"name":"Astronomy and Computing","volume":"49 ","pages":"Article 100891"},"PeriodicalIF":1.9000,"publicationDate":"2024-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"0","resultStr":null,"platform":"Semanticscholar","paperid":null,"PeriodicalName":"Astronomy and Computing","FirstCategoryId":"101","ListUrlMain":"https://www.sciencedirect.com/science/article/pii/S2213133724001069","RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"Q2","JCRName":"ASTRONOMY & ASTROPHYSICS","Score":null,"Total":0}
引用次数: 0

Abstract

Context

Spectral lines of diatomic molecules are perfect tools for studying the structure of sunspots and their temperature layers and magnetic sensitive absorption features, which are typically higher than in atomic lines. The integrated intensities of a few bands in the rotational structure of the astrophysically significant A1Σ+X1Σ+and A1ΠX1Σ+ systems of barium monoxide (BaO) have been measured experimentally using band spectra. An analysis of the prominent lines of (0, 0; 1, 1; 2, 2) bands of A1Σ+X1Σ+transition and (0, 0; 1, 1; 2, 2) bands of A1ΠX1Σ+transition with those of sunspot umbral spectrum. The effective rotational temperatures of the A1ΠX1Σ+transition of BaO in the sunspot umbral spectrum are found to be in the range of 1600 K to 3200 K.

Aims

An analysis of BaO prominent rotational molecular lines of A1Σ+X1Σ+and A1ΠX1Σ+transition with those of sunspot umbral spectral lines. To find the significant values of radiative transition parameters, vibrational temperature and the effective rotational temperature of the molecule in celestial objects.

Methods

Calibrated the rotational structure of molecular band heads and lines for and A1Σ+X1Σ+and A1ΠX1Σ+ransitions in laboratory spectrum using most precise Hartmann's technique. High resolution FTS sunspot umbral spectra from NSO/Kitt Peak were used to detect rotational molecular lines due to the A1ΠX1Σ+transition of the BaO molecule using the method of line coincidence. The effective rotational temperature was derived from the variation of equivalent width (W) with rotational quantum number (J) of spectrally well resolved rotational lines of a band in umbral spectrum. The triangular profile approximation method was used to estimate the equivalent width of the well resolved spectral lines.

Results

The effective rotational temperatures of the A1ΠX1Σ+transition of BaO in the sunspot umbral spectrum are found to be in the range of 1600 K to 3200 K. It is compared with other results with a view to obtaining useful physical parameters. This is an evidence to ascertain the possible presence of BaO molecule in solar spectrum in different layers.

Conclusions

Unblended rotational lines due to the band of BaO, provide a good range of temperatures for the study of absorbing layers in umbral spectra. The A1ΠX1Σ+transition of BaO molecular lines is found to be very sensitive to effective temperature. Radiative transition parameters data of these lines, in contrast to intensity measurements, provide us with more direct and detailed information to study the coolest parts of sunspot umbrae.
关于探测太阳黑子光谱中的氧化钡分子线
背景二原子分子的谱线是研究太阳黑子结构及其温度层和磁敏感吸收特征的完美工具,其吸收率通常高于原子谱线。我们利用波段光谱对一氧化钡(BaO)具有天体物理学意义的 A1Σ+-X1Σ+ 和 A′1Π-X1Σ+ 系统旋转结构中几个波段的综合强度进行了实验测量。分析了 A1Σ+-X1Σ+ 转变的 (0, 0; 1, 1; 2, 2) 波段和 A′1Π-X1Σ+ 转变的 (0, 0; 1, 1; 2, 2) 波段的突出线与太阳黑子本征光谱的突出线。分析了太阳黑子本征光谱中 BaO 的 A′1Π-X1Σ+过渡的 A′1Π-X1Σ+有效旋转温度与太阳黑子本征光谱线的有效旋转温度。方法用最精确的哈特曼技术校准实验室光谱中 A1Σ+-X1Σ+ 和 A′1Π-X1Σ+ 转变的分子带头和线的旋转结构。利用来自 NSO/Kitt Peak 的高分辨率 FTS 太阳黑子本体光谱,采用线重合的方法探测了由于 BaO 分子的 A′1Π-X1Σ+ 转变而产生的旋转分子线。有效旋转温度是根据本征光谱中某一波段的光谱解析旋转线的等效宽度(W)随旋转量子数(J)的变化而得出的。结果发现太阳黑子本影光谱中 BaO 的 A′1Π-X1Σ+ 转变的有效旋转温度在 1600 K 到 3200 K 之间。结论BaO带引起的不混合旋转线为研究本影光谱中的吸收层提供了良好的温度范围。研究发现,BaO 分子线的 A′1Π-X1Σ+ 转变对有效温度非常敏感。与强度测量相比,这些线的辐射转变参数数据为我们研究太阳黑子本影最冷部分提供了更直接、更详细的信息。
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来源期刊
Astronomy and Computing
Astronomy and Computing ASTRONOMY & ASTROPHYSICSCOMPUTER SCIENCE,-COMPUTER SCIENCE, INTERDISCIPLINARY APPLICATIONS
CiteScore
4.10
自引率
8.00%
发文量
67
期刊介绍: Astronomy and Computing is a peer-reviewed journal that focuses on the broad area between astronomy, computer science and information technology. The journal aims to publish the work of scientists and (software) engineers in all aspects of astronomical computing, including the collection, analysis, reduction, visualisation, preservation and dissemination of data, and the development of astronomical software and simulations. The journal covers applications for academic computer science techniques to astronomy, as well as novel applications of information technologies within astronomy.
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