Dust in the Outer Layers of Stars (Record no. 35888)
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| 000 -LEADER | |
|---|---|
| fixed length control field | 02417nam a22001817a 4500 |
| 003 - CONTROL NUMBER IDENTIFIER | |
| control field | OSt |
| 005 - DATE AND TIME OF LATEST TRANSACTION | |
| control field | 20211112113817.0 |
| 008 - FIXED-LENGTH DATA ELEMENTS--GENERAL INFORMATION | |
| fixed length control field | 211112b ||||| |||| 00| 0 eng d |
| 040 ## - CATALOGING SOURCE | |
| Transcribing agency | IIA Library |
| 100 ## - MAIN ENTRY--PERSONAL NAME | |
| Personal name | Dikpati, M. |
| Relator term | Author |
| 9 (RLIN) | 48927 |
| 245 ## - TITLE STATEMENT | |
| Title | Dust in the Outer Layers of Stars |
| Statement of responsibility, etc. | M. Dikpati |
| Medium | [Thesis] |
| 300 ## - PHYSICAL DESCRIPTION | |
| Extent | iii, 165p. |
| 502 ## - DISSERTATION NOTE | |
| Degree type | Doctor of Philosophy |
| Name of granting institution | Karnataka university,Dharwad |
| Year degree granted | 1990 |
| 520 ## - SUMMARY, ETC. | |
| Summary, etc. | We have studied the effects of expansion of dusty<br/>matter in spherically symmetric atmospheres I on equivalent<br/>widths of the spectral lines form in such media. We have<br/>treated a two level atom in non-LTE. Initially the hydrogen<br/>Lyman Alpha line has been studied for the purpose of calculating<br/>the effects of number density of the neutral atoms on<br/>equivalent widths. The temperature variation has been derived<br/>from the assumption that the Planck function varies<br/>as l/r2 in an atmospheres with pure hydrogen gas. Using<br/>this temperature structure and Boltzmann equation I we calculated<br/>the number of neutral atoms which formed the hydrogen<br/>Lyman Alpha Line.<br/>The dust has been introduced assuming that there<br/>is no reemission from the dust and that dust scatters isotropic ally.<br/>This is because the emission of dust will be<br/>in the infrared and will not contribute to the emission<br/>to the hydrogen Lyman<br/>commoving frame method<br/>line transfer equation.<br/>Alpha Line. We have employed the<br/>for obtaining the solution of the<br/>The velocities of expansion are<br/>measured in terms of mean thermal units and the amounts<br/>of gas and dust are measured in terms of the respective<br/>optical depths. We have considered two atmospheres: onewithout<br/>emission and two- with emission in the medium due<br/>to thermalization of photons.<br/>In a static medium we obtain symmetric profiles and<br/>when the velocity of expansion is introduced we generally<br/>obtain P-Cygni type profiles i.e. the absorption being shifted<br/>towards the violet side or emission peak remains at the<br/>center gravity of the line. If we introduce dust the emission<br/>reduce considerably whiIe dust scatters more photons<br/>into the absorpiton core. When there is no dust the absorption<br/>core is very wide extending approximately to three<br/>Doppler units of either side of the center of the lines. |
| 700 ## - ADDED ENTRY--PERSONAL NAME | |
| Personal name | A. Peraiah |
| Relator term | Supervisor |
| 9 (RLIN) | 48850 |
| 856 ## - ELECTRONIC LOCATION AND ACCESS | |
| Uniform Resource Identifier | <a href="http://prints.iiap.res.in/handle/2248/114">http://prints.iiap.res.in/handle/2248/114</a> |
| Link text | Click Here to Access eThesis |
| 942 ## - ADDED ENTRY ELEMENTS (KOHA) | |
| Source of classification or shelving scheme | Universal Decimal Classification |
| Koha item type | Thesis & Dissertations |
| Withdrawn status | Lost status | Source of classification or shelving scheme | Damaged status | Not for loan | Home library | Current library | Shelving location | Date acquired | Total Checkouts | Barcode | Date last seen | Price effective from | Koha item type |
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| Universal Decimal Classification | IIA Library-Bangalore | IIA Library-Bangalore | General Stacks | 21/07/2018 | T019 | 12/11/2021 | 12/11/2021 | Thesis & Dissertations |