{"created":"2023-06-20T13:20:24.883899+00:00","id":429,"links":{},"metadata":{"_buckets":{"deposit":"4363eb8c-99f9-4ead-886f-f67a8b49cfec"},"_deposit":{"created_by":1,"id":"429","owners":[1],"pid":{"revision_id":0,"type":"depid","value":"429"},"status":"published"},"_oai":{"id":"oai:ir.soken.ac.jp:00000429","sets":["2:427:11"]},"author_link":["0","0","0"],"item_1_creator_2":{"attribute_name":"著者名","attribute_type":"creator","attribute_value_mlt":[{"creatorNames":[{"creatorName":"高橋, 智子"}],"nameIdentifiers":[{"nameIdentifier":"0","nameIdentifierScheme":"WEKO"}]}]},"item_1_creator_3":{"attribute_name":"フリガナ","attribute_type":"creator","attribute_value_mlt":[{"creatorNames":[{"creatorName":"タカハシ, サトコ"}],"nameIdentifiers":[{"nameIdentifier":"0","nameIdentifierScheme":"WEKO"}]}]},"item_1_date_granted_11":{"attribute_name":"学位授与年月日","attribute_value_mlt":[{"subitem_dategranted":"2007-03-23"}]},"item_1_degree_grantor_5":{"attribute_name":"学位授与機関","attribute_value_mlt":[{"subitem_degreegrantor":[{"subitem_degreegrantor_name":"総合研究大学院大学"}]}]},"item_1_degree_name_6":{"attribute_name":"学位名","attribute_value_mlt":[{"subitem_degreename":"博士（理学）"}]},"item_1_description_12":{"attribute_name":"要旨","attribute_value_mlt":[{"subitem_description":"In the last two decades, the development of millimeters interferometers has enabled us to establish a standard scenario of sun-like (<i>M</i><sub>*</sub>～1 <i>M</i><small>&Theta;</small> ) star formation. However, details of formation and　evolution of more massive stars (&ge;2 <i>M</i><small>&Theta;</small>, that is, intermediate- and high-mass protostars, remain　poorly understood. Studies of the formation and evolution of intermediate-mass protostars will allow us to understand whether the established low-mass star-formation scenario is applicable to a wide range of protostar masses.　However, there is no systematic observation toward　interemediate-mass protostars. It is important to directly verify the accretion and dissipation (or destruction) processes of dense gas envelopes around intermediate-mass protostars. For these　purpose, The author has performed multi-wavelength and multi-line survey observations toward intermediate-mass pre- and proto-stellar candidates in the Orion Molecular Cloud -2/3 region 　(OMC- 2/3）. The OMC- 2/3 region is one of the best targets to conduct asystematic survey of　intermediate-mass protostars, because all of the sources are in the same distance and under the　similar starforming environment.<br /><br />　　Using the NMA, ASTE and SIRIUS / IRSF, The author observed the 3.3 mm dust continuum,　H<sup>13</sup>CO<sup>＋</sup>(1-0), CO(1-0), CO(3-2) emissions, and near infrared (<i>JHK<small>s</small></i> band) continuum emissions　toward the entire sample of intermediate-mass pre- and proto-stellar candidates in the Orion　Molecular Cloud-2/3 region (OMC-2/3). Based on our H<sup>13</sup>CO<sup>＋</sup>(1-0), 3.3 mm continuum,　CO(3-2) and <i>JHK<small>s</small></i> results, combined with the published VLA 3.6 cm and the archived 24　<i>mu</i>m data taken by Spitzer, The author unveiled the evolutionary changes, morphology and　velocity structures of the dense envelopes and accompanied CO outflows around intermediate-mass　protostars for the first time. The author classified these intermediate-mass pre- and proto-stellar　candidates into three evolutionary phases as (i) pre-stellar phase, (ii) Class A phase, and (iii)　Class B phase. Pre-stellar sources have no compact dusty emission taken with the NMA and 24　μm　source, suggesting no any signature of dense (>10<sup>7</sup>cm<sup>-3</sup>) and hot (>100 K) envelopes. In　this phase, there are no signature of jets/outflows. Class A sources are corresponding to the earlier　evolutionary phase of the protosterllar cores, which are associated with compact dust emission and　24μm sources, suggesting the presence of the heating source. 0.1 pc scale CO outflows are also　detected in this phase.  Finally, Class B sources correspond to the later evolutionary phase of the protostellar cores, which are associated with the compact dust and 24 μm sources. 0.5-1.0　pc scale CO outflow and free-free jet are associated with these objects. In addition, our <i>JHK</i><small>s</small>　images show a reflection nebula, suggesting the formation of the cavity along the CO outflows. In　this phase, the author detected fan-shaped H<sup>13</sup>CO<sup>＋</sup> envelops with a size scale of 0.1 pc.<br /><br />　　The author also found that the CO outflow momentum increases from the evolutionary　sequence of Class A to Class B. The 24 μm peak flux also increases from the evolutionary sequence　of Class A to Class B. The author suggests that the enhancement of the 24 μm flux is caused by 　the growth of the cavity (i.e., the CO outflow destroys the envelope) as the evolutionary sequence.　Our results show that the dissipation of the dense gas envelope plays an essential role in the　evolution of the intermediate-mass protostars.","subitem_description_type":"Other"}]},"item_1_description_7":{"attribute_name":"学位記番号","attribute_value_mlt":[{"subitem_description":"総研大甲第1033号","subitem_description_type":"Other"}]},"item_1_select_14":{"attribute_name":"所蔵","attribute_value_mlt":[{"subitem_select_item":"有"}]},"item_1_select_8":{"attribute_name":"研究科","attribute_value_mlt":[{"subitem_select_item":"物理科学研究科"}]},"item_1_select_9":{"attribute_name":"専攻","attribute_value_mlt":[{"subitem_select_item":"09 天文科学専攻"}]},"item_1_text_10":{"attribute_name":"学位授与年度","attribute_value_mlt":[{"subitem_text_value":"2006"}]},"item_creator":{"attribute_name":"著者","attribute_type":"creator","attribute_value_mlt":[{"creatorNames":[{"creatorName":"TAKAHASHI, Satoko","creatorNameLang":"en"}],"nameIdentifiers":[{"nameIdentifier":"0","nameIdentifierScheme":"WEKO"}]}]},"item_files":{"attribute_name":"ファイル情報","attribute_type":"file","attribute_value_mlt":[{"accessrole":"open_date","date":[{"dateType":"Available","dateValue":"2016-02-17"}],"displaytype":"simple","filename":"甲1033_要旨.pdf","filesize":[{"value":"295.2 kB"}],"format":"application/pdf","licensetype":"license_11","mimetype":"application/pdf","url":{"label":"要旨・審査要旨","url":"https://ir.soken.ac.jp/record/429/files/甲1033_要旨.pdf"},"version_id":"db49de5c-a952-420d-ac15-fee40490da6c"},{"accessrole":"open_date","date":[{"dateType":"Available","dateValue":"2016-02-17"}],"displaytype":"simple","filename":"甲1033_本文.pdf","filesize":[{"value":"39.2 MB"}],"format":"application/pdf","licensetype":"license_11","mimetype":"application/pdf","url":{"label":"本文","url":"https://ir.soken.ac.jp/record/429/files/甲1033_本文.pdf"},"version_id":"53d64d09-e970-415d-b880-0b60ce25bf00"}]},"item_language":{"attribute_name":"言語","attribute_value_mlt":[{"subitem_language":"eng"}]},"item_resource_type":{"attribute_name":"資源タイプ","attribute_value_mlt":[{"resourcetype":"thesis","resourceuri":"http://purl.org/coar/resource_type/c_46ec"}]},"item_title":"Structure and Evolution of Intermediate-mass Protostars","item_titles":{"attribute_name":"タイトル","attribute_value_mlt":[{"subitem_title":"Structure and Evolution of Intermediate-mass Protostars"},{"subitem_title":"Structure and Evolution of Intermediate-mass Protostars","subitem_title_language":"en"}]},"item_type_id":"1","owner":"1","path":["11"],"pubdate":{"attribute_name":"公開日","attribute_value":"2010-02-22"},"publish_date":"2010-02-22","publish_status":"0","recid":"429","relation_version_is_last":true,"title":["Structure and Evolution of Intermediate-mass Protostars"],"weko_creator_id":"1","weko_shared_id":1},"updated":"2023-06-20T16:02:12.760038+00:00"}