{"created":"2023-06-20T13:20:24.971494+00:00","id":431,"links":{},"metadata":{"_buckets":{"deposit":"96e97cc5-e736-475a-b7f0-d55d3cab693b"},"_deposit":{"created_by":1,"id":"431","owners":[1],"pid":{"revision_id":0,"type":"depid","value":"431"},"status":"published"},"_oai":{"id":"oai:ir.soken.ac.jp:00000431","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":"西川, 貴行"}],"nameIdentifiers":[{"nameIdentifier":"0","nameIdentifierScheme":"WEKO"}]}]},"item_1_creator_3":{"attribute_name":"フリガナ","attribute_type":"creator","attribute_value_mlt":[{"creatorNames":[{"creatorName":"ニシカワ, タカユキ"}],"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":"Optical jets and molecular bipolar outflows are two major manifestations<br />of outflowing activities associated with young stellar objects （YSOs）．It is<br />not clear how these two outflow activities are related with each other．One of<br />the major scenarios is that a collimated jet seen in the optical－IR wavelength<br />entrains its ambient molecular material，a1lowing the molecular outflow to<br />occur. In order for us to tackle this issue，it is crucial to understand how jets<br />interact with ambient material．<br />　In addition to the kinematics，the mass loss rate and mass momentum<br />transfer rate of are key parameters to investigate how the jet interacts<br />with the ambient material.　However，the mass momentum is poorly known<br />because the hydrogen density is not easily derived， as is different from the<br />electron density that is measured  from forbidden line emissions． If we assume<br />that a jet is fully ionized, i.e. the electron density is nearly equal to the<br />hydrogen density，the mass momentum of the jet derived from its optical<br />emission lines is not sufficient to drive the molecular outflow associated with<br />it. In contrast，recent studies have suggested that jets are almost neutral，<br />indicating that a jet may have momentum sufficient to drive a molecular outflow．<br />　　In order to study the issues described above，we made slit-scan observa-<br />tions of Hα and [NII] 6583 &Aring; emission lines toward two bright jets，HH46/47<br />and the HL Tau jet，with Subaru Telescope. The large diameter of the tele-<br />scope，together with the high spectral resolution of the spectrograph（High<br />Dispersion Spectrograph，R =3.6×10<sup>40</sup> or &Delta;v＝8km s<sup>-1</sup>）allowed us to<br />study the kinematics of these jets in unprecedented detail．Furthermore，the<br />slit-scan technique with a long slit provided us with kinematic information<br />of the entire jets．<br />　　We found that，in both jets，the Hα emission traces both the main jet<br />component（<i>V</i><small>LSR</small>＝－160～－180km s<sup>-1</sup>）and distinct lower velocity com-<br />ponent （|<i>V</i><small>LSR</small>| &le; 120km s<sup>-1</sup>）.　The [NII] emission, on the other hand，is<br />primarily associated with the main jet component and is much faint or ab－<br />sent in the lower velocity component. 　In the HH 46/47 jet，the velocities<br />of Hαand [NII] emission lines match well in their main jet components．<br />The lower velocity components are associated with one-sided bow shocks<br />and with one of the Hα filaments that was previous identified with the<br /><i>Hubble Space Telescope.</i>　In　the　HL　Tau　jet，the　lower　velocity　component<br />is associated with indivisual knots, which is explained by the lower velocity<br />emmituion arising  in the laterals of bow shocks. While the main jet component<br />is associated with the ejecta, the lower velocity component is produced as a<br />result of the interaction between the ejecta and the surrounding gas.<br />　　Observed Hα line profiles suggest that the shock velocities at the bow<br />shocks and the Hα filament with respect to the ambient gas are 60－80km s<sup>-1</sup><br />and 120－130 km s<sup>-1</sup> for HH46/47 and HL Tau，respectively.　These are<br />markedly smaller than the three dimensional（3－D）velocities of the jets（～300<br />km s<sup>-1</sup>）．　　The discrepancy between the shock velocity and 3－D velocity is<br />explained if the ambient gas moves outward by～200km s<sup>-1.</sup>.　The velocity<br />of the ambient gas measured in the HH46/47 jet is similar to those of HH<br />47A and 47D，giant bow shocks ahead of the observed region.<br />　　Through detailed analysis，we concluded that the outward motion of the<br /> ambient gas is a result of prompt entrainment，i．e. a jet sweeps up ambient<br />material at its head by a large bow shock，but not of turbulent entrainment，<br />the other entrainment mechanism proposed to date．Indeed，our high spec-<br />tral resolution slit-scan observations of Hαshow that the main jet component<br />has a uniform radial velocity of <i>V</i><small>LSR</small>＝－160km s<sup>-1</sup>（&Delta;v＝10km s<sup>-1</sup>）and<br />did not show the presence of slow Hα components（ |<i>V</i><small>LSR</small> | &le; 120km s-<sup>1</sup>）<br />along the edges of the jets．Such slow Hα emission was reported in previous<br />observations and was proposed to arise from turbulent boundary layers be-<br />tween the main flow and the ambient gas.　Our results indicate that Hα and<br />[NII] originate from the main jet component（i．e. the ejecta），and also from<br />bow shocks and Hα filaments，but not from turbulent mixing layers.<br />　　 We also investigated the ionization fraction in the jets using the [NII] / Hα<br />flux ratio.　In the　case　of　HH46/47，the ratio is 0.2-0.5 in the main jet<br />component and even higher in some other regions．Shock model calculations<br />show that the ratio is sensitive to the ionization fraction of preshock gas if<br />the shock velocity is less than l00 km s<sup>-1</sup>．　The　observed　high　ratio　for HH<br />46/47 is expected if its main jet component is considerably ionized，although<br />previous observations proposed a much lower ionization fraction of&le;0.2．<br />The [NII] / Hαflux ratio is significantly smaller than 0.2  in the one-side bow<br />shocks and Hα filaments, indicating that the gas surrounding the ejecta is<br />rather neutral．<br />　　For the HL Tau jet，the observed [NII] / Hα flux ratio markedly vary from<br />one region to another: 0.1-0.7 at the base of the jet，less than 0.1 in knot<br />A，～0.2 in knot B，～0.4 in knot C，and ～0.7 in knot D．Because the shock<br/>velocities of the HL Tau jet exceed 100 km s<sup>-1</sup> in some regions，the ratio<br />does not directly reflect the ionization fraction of preshock gas. At the knots<br />A－D，the [NII] / Hαflux ratio increases from ＜0.1 to 0.7 with distance from<br />the source. This suggests that the preshock density decreases with distance<br />from the source．The ratio at the lateral of the bow shocks is less than<br />～0.1，suggesting that the ambient medium is almost neutral．At the base<br />of the jet，the observed  [NII] / Hα flux ratio decreases from 0.7 to 0.1 as the<br />distance from the source increase. This suggests that the ionization fraction<br />decreases with distance as a result of radiative recombination．<br />　　We compared the [NII] / Hα ratio in the main jet components of the HH<br />46/47 jet and HL Tau jet. The ratio for the HH 46/47 jet is higher（0.2－0.5）<br />than that for the HL Tau（&le; 0.2），indicating high ionization fraction．Such<br />a difference suggests that the radiation from a nearby O star irradiates the<br />ambient gas of the HH 46/47 system，which is located near the HII region<br />Gum nebula，causing the high ionization fraction in the main jet component．<br />Another possible interpretation is that radiative cooling by recombination is<br />not efficient in the HH 46/47 jet because of its low density，thus allowing the<br />high ionization fraction in the jet significantly away from the driving source．","subitem_description_type":"Other"}]},"item_1_description_18":{"attribute_name":"フォーマット","attribute_value_mlt":[{"subitem_description":"application/pdf","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1035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":"NISHIKAWA, Takayuki","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1035_要旨.pdf","filesize":[{"value":"382.0 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/431/files/甲1035_要旨.pdf"},"version_id":"241db0af-4181-4123-bb71-d6695aed5cd9"},{"accessrole":"open_date","date":[{"dateType":"Available","dateValue":"2016-02-17"}],"displaytype":"simple","filename":"甲1035_本文.pdf","filesize":[{"value":"24.5 MB"}],"format":"application/pdf","licensetype":"license_11","mimetype":"application/pdf","url":{"label":"本文","url":"https://ir.soken.ac.jp/record/431/files/甲1035_本文.pdf"},"version_id":"147962ac-4eb9-4bbf-b037-149e7b57fa31"}]},"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":"Kinematic Structure and Ionization of  Optical Jets Associated with Young Stellar Objects","item_titles":{"attribute_name":"タイトル","attribute_value_mlt":[{"subitem_title":"Kinematic Structure and Ionization of  Optical Jets Associated with Young Stellar Objects"},{"subitem_title":"Kinematic Structure and Ionization of  Optical Jets Associated with Young Stellar Objects","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":"431","relation_version_is_last":true,"title":["Kinematic Structure and Ionization of  Optical Jets Associated with Young Stellar Objects"],"weko_creator_id":"1","weko_shared_id":-1},"updated":"2023-06-20T16:13:27.635493+00:00"}