Stellar atmospheres

Part 1 — TABLE XIII

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STELLAR ATMOSPHERES EDITOR’S FOREWORD

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TABLE I TABLE II TABLE III TABLE IV

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TABLE V TABLE VI TABLE VII TABLE VIII TABLE IX

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TABLE XVII

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7 8

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TABLEXVIII TABLE XIX NOTES ON OBSERVATIONAL MATERIAL

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TABLE XX TABLE XXI TABLE XXII

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TABLE XXIII TABLE XXIV

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TABLE XXV

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TABLE XXVI

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TABLE XXVII TABLE XXVIII TABLE XXIX

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TABLE XXX TABLE XXXI

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APPENDICES

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TABLE XXXII TABLE XXXIII TABLE XXXIV SUBJECT INDEX NAME INDEX

Series Wave-Lenght Int. Attribution Int. Wave-Lenght

3328.34 3 1 3328.487

3336.33 5 Cr 2 3336.477

3324.06 3 3324.19

3339.80 10 Co, Cr 3 3339.932

3347.83 6 Cr 3 3347.970

3342.58 10 Cr 3 3342.717

3358.50 10 Ti, Cr 4 3358.649

3368.04 20 Cr, - ? 3368.193

3132.04 20 -, Cr 4 3132.169

3124.97 20 Cr 4 3125.109

3147.22 5 Cr 3 3147.350

3120.36 15 Cr, - 3 3120.481

3136.69 5 Cr, Co 3 3136.822

3159.10 1 0 3159.225

3118.65 10 Cr, - 2 3118.764

3128.68 5 Cr, - 2 3128.819

3145.07 2 2 3145.251

MANGANESE (25)

The lines of manganese are conspicuous in stellar spectra, and all the classified lines[312] within the range of Rowland’s table are found in the solar spectrum, namely the multiplets , , , , , , , , , . The ultimate lines are at 4030, and constitute a conspicuous group in the solar spectrum. They are well seen in the cooler stars, and are progressively strengthened with advancing type.[313] They first appear at . The multiplet, at 4018, 4041, 4055, 4084, etc., has a maximum, according to Menzel,[314] at .

IONIZED MANGANESE

Meggers, Kiess, and Walters[315] give one multiplet of ionized manganese, and this is within the range of Rowland’s table. The multiplet was previously picked out by Catalan[316] as being analogous to the arc multiplet . All the lines can be satisfactorily identified with lines in the solar spectrum, as in the following table.

Notes in this chapter

Note 1 · Catalan, Phil. Trans., 223A, 127, 1922.Note 2 · Chapter VIII, p. 124.Note 3 · H. C. 238, 1924.Note 4 · J. Op. Soc. Am., 9, 355, 1924.Note 5 · Phil. Trans., 223A, 127, 1922.