| DC 欄位 |
值 |
語言 |
| DC.contributor | 天文研究所 | zh_TW |
| DC.creator | 劉芳君 | zh_TW |
| DC.creator | Fang-Chun Liu | en_US |
| dc.date.accessioned | 2009-7-22T07:39:07Z | |
| dc.date.available | 2009-7-22T07:39:07Z | |
| dc.date.issued | 2009 | |
| dc.identifier.uri | http://ir.lib.ncu.edu.tw:88/thesis/view_etd.asp?URN=962209006 | |
| dc.contributor.department | 天文研究所 | zh_TW |
| DC.description | 國立中央大學 | zh_TW |
| DC.description | National Central University | en_US |
| dc.description.abstract | 我們利用多波段觀測來研究兩個在巴納德星雲的毫米/次毫米天體，他們的名稱是Barnard 1-bN和Barnard 1-bS。從這兩個天體所發出的塵埃連續輻射訊號，我們發現他們物質分布很緻密，且物質本身相當低溫（塵埃溫度10-16 K）。Spitzer的MIPS望遠鏡所拍出的24和60微米波段影像裡，這兩個天體並沒有被偵測到，這表示他們還包裹在雲深處。由SMA觀測的CO（J=2-1）譜線資料顯現出Barnard 1-bS有噴流，Barnard 1-bN則是疑似有噴流。這些噴流都不是很大（大約2000 AU大小）。這個結果指出這兩個天體已經蘊含著Class 0原恆星。另一方面，這兩個天體的化學特性反而相似於前恆星核：N2D+（J=3-2）譜線訊號很強而且和塵埃連續輻射訊號的分布很一致。反之，H13CO+（J=1-0）譜線訊號則很微弱，甚至是沒有偵測到。這樣的化學特性可能是因為在低溫高密度環境中，H13CO+ 分子已經分解附著在塵粒上所導致。而這樣子的化學特性是相似於前恆星核的化學特性。因此，綜合我們所發現的這兩個天體的物理及化學特性，我們可以知道Barnard 1-bN和Barnard 1-bS是在恆星形成非常早期的天體，他們的演化時期可能正好落在前恆星核時期與Class 0原恆星時期中間。
| zh_TW |
| dc.description.abstract | The physical and chemical properties of two mm/sub-mm sources in Barnard cloud, Barnard 1-bN and Barnard 1-bS, are studied with multi-wavelength observations. The dust continuum from these two sources shows spatially compact distribution and very cold spectral energy distributions (T$_{dust}$=10--16 K). These two sources have no mid-IR counterpart in the Spitzer MIPS 24 and 60 micron bands, indicating that they are deeply embedded. The CO J=2--1 data obtained with the SMA suggest that B1-bS and probably B1-bN are associated with the compact ($sim$ 2000; AU size) molecular outflows. These results suggest that Barnard 1-bN and Barnard 1-bS are already harboring Class 0 protostars. On the other hand, the chemical properties of these two sources are similar to those of pre-stellar cores: the N$_2$D$^+$ J=3--2 emission is strong (0.3 K for B1-bN and 0.1 K for B1-bS) and clearly traces the two compact sources, while the H$^{13}$CO$^+$ J=1--0 emission is weak or barely detected near or at the continuum peaks. This lack of H$^{13}$CO$^+$ emission is probably due to the depletion of the H$^{13}$CO$^+$ molecule onto the grain under the condition of low temperature and high density, as in the case of pre-stellar cores. The observed physical and chemical properties suggest that B1-bN and B1-bS are in the very beginning stage of protostellar evolution, probably in the evolutionary stage between pre-stellar core and class 0 source.
| en_US |
| DC.subject | 恆星形成 | zh_TW |
| DC.subject | 原恆星 | zh_TW |
| DC.subject | star formation | en_US |
| DC.subject | Class 0 | en_US |
| DC.subject | protostar | en_US |
| DC.subject | prestellar core | en_US |
| DC.title | Millimeter and Submillimeter Observations of Barnard 1-bN and Barnard 1-bS | en_US |
| dc.language.iso | en_US | en_US |
| DC.type | 博碩士論文 | zh_TW |
| DC.type | thesis | en_US |
| DC.publisher | National Central University | en_US |