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(PDF) High-mass Star Formation through Filamentary Collapse and Clump-fed Accretion in G22
<!DOCTYPE html> <html > <head> <meta charset="utf-8"> <meta rel="search" type="application/opensearchdescription+xml" href="/open_search.xml" title="Academia.edu"> <meta content="width=device-width, initial-scale=1" name="viewport"> <meta name="google-site-verification" content="bKJMBZA7E43xhDOopFZkssMMkBRjvYERV-NaN4R6mrs"> <meta name="csrf-param" content="authenticity_token" /> <meta name="csrf-token" content="8sPnQO--JBfz02TT7jHBD8YCPZNvUEFf8n5W9csIGDqqnHn1KkrhFwRGqqgkyLYWO9RV9HJnAW60I7-dU-mqQA" /> <meta name="citation_title" content="High-mass Star Formation through Filamentary Collapse and Clump-fed Accretion in G22" /> <meta name="citation_publication_date" content="2017" /> <meta name="citation_journal_title" content="The Astrophysical Journal" /> <meta name="citation_author" content="Jinghua Yuan" /> <meta name="citation_author" content="Jin-Zeng Li" /> <meta name="citation_author" content="Yuefang Wu" /> <meta name="citation_author" content="Simon P. Ellingsen" /> <meta name="citation_author" content="Christian Henkel" /> <meta name="citation_author" content="Ke Wang" /> <meta name="citation_author" content="Tie Liu" /> <meta name="citation_author" content="Hong-Li Liu" /> <meta name="citation_author" content="Annie Zavagno" /> <meta name="citation_author" content="Zhiyuan Ren" /> <meta name="citation_author" content="Ya-Fang Huang" /> <meta name="citation_volume" content="852" /> <meta name="citation_issue" content="1" /> <meta name="citation_firstpage" content="12" /> <meta name="citation_issn" content="1538-4357" /> <meta name="twitter:card" content="summary" /> <meta name="twitter:url" content="https://www.academia.edu/35538530/High_mass_Star_Formation_through_Filamentary_Collapse_and_Clump_fed_Accretion_in_G22" /> <meta name="twitter:title" content="High-mass Star Formation through Filamentary Collapse and Clump-fed Accretion in G22" /> <meta name="twitter:description" content="How mass is accumulated from cloud-scale down to individual stars is a key open question in understanding high-mass star formation. Here, we present the mass accumulation process in a hub-filament cloud G22 that is composed of four supercritical" /> <meta name="twitter:image" content="https://0.academia-photos.com/66695878/17364443/17484885/s200_jinghua.yuan.jpg" /> <meta property="fb:app_id" content="2369844204" /> <meta property="og:type" content="article" /> <meta property="og:url" content="https://www.academia.edu/35538530/High_mass_Star_Formation_through_Filamentary_Collapse_and_Clump_fed_Accretion_in_G22" /> <meta property="og:title" content="High-mass Star Formation through Filamentary Collapse and Clump-fed Accretion in G22" /> <meta property="og:image" content="http://a.academia-assets.com/images/open-graph-icons/fb-paper.gif" /> <meta property="og:description" content="How mass is accumulated from cloud-scale down to individual stars is a key open question in understanding high-mass star formation. Here, we present the mass accumulation process in a hub-filament cloud G22 that is composed of four supercritical" /> <meta property="article:author" content="https://gucas.academia.edu/jhyuannaoc" /> <meta name="description" content="How mass is accumulated from cloud-scale down to individual stars is a key open question in understanding high-mass star formation. Here, we present the mass accumulation process in a hub-filament cloud G22 that is composed of four supercritical" /> <title>(PDF) High-mass Star Formation through Filamentary Collapse and Clump-fed Accretion in G22</title> <link rel="canonical" href="https://www.academia.edu/35538530/High_mass_Star_Formation_through_Filamentary_Collapse_and_Clump_fed_Accretion_in_G22" /> <script async src="https://www.googletagmanager.com/gtag/js?id=G-5VKX33P2DS"></script> <script> window.dataLayer = window.dataLayer || []; function gtag(){dataLayer.push(arguments);} gtag('js', new Date()); gtag('config', 'G-5VKX33P2DS', { cookie_domain: 'academia.edu', send_page_view: false, }); gtag('event', 'page_view', { 'controller': "single_work", 'action': "show", 'controller_action': 'single_work#show', 'logged_in': 'false', 'edge': 'unknown', // Send nil if there is no A/B test bucket, in case some records get logged // with missing data - that way we can distinguish between the two cases. // ab_test_bucket should be of the form <ab_test_name>:<bucket> 'ab_test_bucket': null, }) </script> <script> var $controller_name = 'single_work'; var $action_name = "show"; var $rails_env = 'production'; var $app_rev = '4fa2af9c4f363dba70f41e510d9d86aae76f6ed9'; var $domain = 'academia.edu'; var $app_host = "academia.edu"; var $asset_host = "academia-assets.com"; var $start_time = new Date().getTime(); var $recaptcha_key = "6LdxlRMTAAAAADnu_zyLhLg0YF9uACwz78shpjJB"; var $recaptcha_invisible_key = "6Lf3KHUUAAAAACggoMpmGJdQDtiyrjVlvGJ6BbAj"; var $disableClientRecordHit = false; </script> <script> window.require = { config: function() { return function() {} } } </script> <script> window.Aedu = window.Aedu || {}; window.Aedu.hit_data = null; window.Aedu.serverRenderTime = new Date(1740155707000); window.Aedu.timeDifference = new Date().getTime() - 1740155707000; </script> <script type="application/ld+json">{"@context":"https://schema.org","@type":"ScholarlyArticle","abstract":"How mass is accumulated from cloud-scale down to individual stars is a key open question in understanding high-mass star formation. Here, we present the mass accumulation process in a hub-filament cloud G22 that is composed of four supercritical filaments. Velocity gradients detected along three filaments indicate that they are collapsing with a total mass infall rate of about 440 M e Myr −1 , suggesting the hub mass would be doubled in six free-fall times, adding up to ∼2 Myr. A fraction of the masses in the central clumps C1 and C2 can be accounted for through large-scale filamentary collapse. Ubiquitous blue profiles in HCO + (3–2) and 13 CO(3–2) spectra suggest a clump-scale collapse scenario in the most massive and densest clump C1. The estimated infall velocity and mass infall rate are 0.31 km s −1 and 7.2×10 −4 M e yr −1 , respectively. In clump C1, a hot molecular core (SMA1) is revealed by the Submillimeter Array observations and an outflow-driving high-mass protostar is located at the center of SMA1. The mass of the protostar is estimated to be 11–15 M e and it is still growing with an accretion rate of 7×10 −5 M e yr −1. The coexistent infall in filaments, clump C1, and the central hot core in G22 suggests that pre-assembled mass reservoirs (i.e., high-mass starless cores) may not be required to form high-mass stars. In the course of high-mass star formation, the central protostar, the core, and the clump can simultaneously grow in mass via core-fed/disk accretion, clump-fed accretion, and filamentary/cloud collapse.","author":[{"@context":"https://schema.org","@type":"Person","name":"Jinghua Yuan","url":"https://gucas.academia.edu/jhyuannaoc"}],"contributor":[],"dateCreated":"2017-12-29","dateModified":"2017-12-29","datePublished":"2018-01-01","headline":"High-mass Star Formation through Filamentary Collapse and Clump-fed Accretion in G22","identifier":{"@type":"PropertyValue","propertyID":"DOI","value":"10.3847/1538-4357/aa9d40"},"image":"https://attachments.academia-assets.com/55404248/thumbnails/1.jpg","inLanguage":"en","keywords":["Star Formation","Star formation (Physics)","Massive Star Formation","Interstellar Medium and Star formation"],"publication":"The Astrophysical 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false; window.loswp.work = {"work":{"id":35538530,"created_at":"2017-12-29T17:29:23.908-08:00","from_world_paper_id":null,"updated_at":"2021-01-16T01:01:10.968-08:00","_data":{"doi":"10.3847/1538-4357/aa9d40","volume":"852","abstract":"How mass is accumulated from cloud-scale down to individual stars is a key open question in understanding high-mass star formation. Here, we present the mass accumulation process in a hub-filament cloud G22 that is composed of four supercritical filaments. Velocity gradients detected along three filaments indicate that they are collapsing with a total mass infall rate of about 440 M e Myr −1 , suggesting the hub mass would be doubled in six free-fall times, adding up to ∼2 Myr. A fraction of the masses in the central clumps C1 and C2 can be accounted for through large-scale filamentary collapse. Ubiquitous blue profiles in HCO + (3–2) and 13 CO(3–2) spectra suggest a clump-scale collapse scenario in the most massive and densest clump C1. The estimated infall velocity and mass infall rate are 0.31 km s −1 and 7.2×10 −4 M e yr −1 , respectively. In clump C1, a hot molecular core (SMA1) is revealed by the Submillimeter Array observations and an outflow-driving high-mass protostar is located at the center of SMA1. The mass of the protostar is estimated to be 11–15 M e and it is still growing with an accretion rate of 7×10 −5 M e yr −1. The coexistent infall in filaments, clump C1, and the central hot core in G22 suggests that pre-assembled mass reservoirs (i.e., high-mass starless cores) may not be required to form high-mass stars. In the course of high-mass star formation, the central protostar, the core, and the clump can simultaneously grow in mass via core-fed/disk accretion, clump-fed accretion, and filamentary/cloud collapse.","page_numbers":"12","publication_date":"2018,,","publication_name":"The Astrophysical Journal"},"document_type":"paper","pre_hit_view_count_baseline":null,"quality":"high","language":"en","title":"High-mass Star Formation through Filamentary Collapse and Clump-fed Accretion in G22","broadcastable":true,"draft":false,"has_indexable_attachment":true,"indexable":true}}["work"]; window.loswp.workCoauthors = [66695878]; window.loswp.locale = "en"; window.loswp.countryCode = "SG"; window.loswp.cwvAbTestBucket = ""; window.loswp.designVariant = "ds_vanilla"; window.loswp.fullPageMobileSutdModalVariant = "full_page_mobile_sutd_modal"; window.loswp.useOptimizedScribd4genScript = false; window.loginModal = {}; window.loginModal.appleClientId = 'edu.academia.applesignon'; window.userInChina = "false";</script><script defer="" src="https://accounts.google.com/gsi/client"></script><div class="ds-loswp-container"><div class="ds-work-card--grid-container"><div class="ds-work-card--container js-loswp-work-card"><div class="ds-work-card--cover"><div class="ds-work-cover--wrapper"><div class="ds-work-cover--container"><button class="ds-work-cover--clickable js-swp-download-button" data-signup-modal="{"location":"swp-splash-paper-cover","attachmentId":55404248,"attachmentType":"pdf"}"><img alt="First page of “High-mass Star Formation through Filamentary Collapse and Clump-fed Accretion in G22”" class="ds-work-cover--cover-thumbnail" src="https://0.academia-photos.com/attachment_thumbnails/55404248/mini_magick20220702-29404-5lrt9k.png?1656752509" /><img alt="PDF Icon" class="ds-work-cover--file-icon" src="//a.academia-assets.com/images/single_work_splash/adobe_icon.svg" /><div class="ds-work-cover--hover-container"><span class="material-symbols-outlined" style="font-size: 20px" translate="no">download</span><p>Download Free PDF</p></div><div class="ds-work-cover--ribbon-container">Download Free PDF</div><div class="ds-work-cover--ribbon-triangle"></div></button></div></div></div><div class="ds-work-card--work-information"><h1 class="ds-work-card--work-title">High-mass Star Formation through Filamentary Collapse and Clump-fed Accretion in G22</h1><div class="ds-work-card--work-authors ds-work-card--detail"><a class="ds-work-card--author js-wsj-grid-card-author ds2-5-body-md ds2-5-body-link" data-author-id="66695878" href="https://gucas.academia.edu/jhyuannaoc"><img alt="Profile image of Jinghua Yuan" class="ds-work-card--author-avatar" src="https://0.academia-photos.com/66695878/17364443/17484885/s65_jinghua.yuan.jpg" />Jinghua Yuan</a></div><div class="ds-work-card--detail"><p class="ds-work-card--detail ds2-5-body-sm">2018, The Astrophysical Journal</p><a class="js-loswp-work-card-doi-link ds2-5-body-sm ds2-5-body-link" href="https://doi.org/10.3847/1538-4357/aa9d40" rel="nofollow">https://doi.org/10.3847/1538-4357/aa9d40</a><div class="ds-work-card--work-metadata"><div class="ds-work-card--work-metadata__stat"><span class="material-symbols-outlined" style="font-size: 20px" translate="no">visibility</span><p class="ds2-5-body-sm" id="work-metadata-view-count">…</p></div><div class="ds-work-card--work-metadata__stat"><span class="material-symbols-outlined" style="font-size: 20px" translate="no">description</span><p class="ds2-5-body-sm">16 pages</p></div><div class="ds-work-card--work-metadata__stat"><span class="material-symbols-outlined" style="font-size: 20px" translate="no">link</span><p class="ds2-5-body-sm">1 file</p></div></div><script>(async () => { const workId = 35538530; 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if (!viewCountBody) { throw new Error('Failed to find work views element'); } viewCountBody.textContent = `${commaizedViewCount} views`; } catch (error) { // Remove the whole views element if there was some issue parsing. document.getElementById('work-metadata-view-count')?.parentNode?.remove(); throw new Error(`Failed to parse view count: ${viewCount}`, error); } }; // If the DOM is still loading, wait for it to be ready before updating the view count. if (document.readyState === "loading") { document.addEventListener('DOMContentLoaded', () => { updateViewCount(viewCount); }); // Otherwise, just update it immediately. } else { updateViewCount(viewCount); } })();</script></div><p class="ds-work-card--work-abstract ds-work-card--detail ds2-5-body-md">How mass is accumulated from cloud-scale down to individual stars is a key open question in understanding high-mass star formation. Here, we present the mass accumulation process in a hub-filament cloud G22 that is composed of four supercritical filaments. Velocity gradients detected along three filaments indicate that they are collapsing with a total mass infall rate of about 440 M e Myr −1 , suggesting the hub mass would be doubled in six free-fall times, adding up to ∼2 Myr. A fraction of the masses in the central clumps C1 and C2 can be accounted for through large-scale filamentary collapse. Ubiquitous blue profiles in HCO + (3–2) and 13 CO(3–2) spectra suggest a clump-scale collapse scenario in the most massive and densest clump C1. The estimated infall velocity and mass infall rate are 0.31 km s −1 and 7.2×10 −4 M e yr −1 , respectively. In clump C1, a hot molecular core (SMA1) is revealed by the Submillimeter Array observations and an outflow-driving high-mass protostar is located at the center of SMA1. The mass of the protostar is estimated to be 11–15 M e and it is still growing with an accretion rate of 7×10 −5 M e yr −1. The coexistent infall in filaments, clump C1, and the central hot core in G22 suggests that pre-assembled mass reservoirs (i.e., high-mass starless cores) may not be required to form high-mass stars. In the course of high-mass star formation, the central protostar, the core, and the clump can simultaneously grow in mass via core-fed/disk accretion, clump-fed accretion, and filamentary/cloud collapse.</p><div class="ds-work-card--button-container"><button class="ds2-5-button js-swp-download-button" data-signup-modal="{"location":"continue-reading-button--work-card","attachmentId":55404248,"attachmentType":"pdf","workUrl":"https://www.academia.edu/35538530/High_mass_Star_Formation_through_Filamentary_Collapse_and_Clump_fed_Accretion_in_G22"}">See full PDF</button><button class="ds2-5-button ds2-5-button--secondary js-swp-download-button" data-signup-modal="{"location":"download-pdf-button--work-card","attachmentId":55404248,"attachmentType":"pdf","workUrl":"https://www.academia.edu/35538530/High_mass_Star_Formation_through_Filamentary_Collapse_and_Clump_fed_Accretion_in_G22"}"><span class="material-symbols-outlined" style="font-size: 20px" translate="no">download</span>Download PDF</button></div><div class="ds-signup-banner-trigger-container"><div class="ds-signup-banner-trigger ds-signup-banner-trigger-control"></div></div><div class="ds-signup-banner ds-signup-banner-control"><div id="ds-signup-banner-close-button"><button class="ds2-5-button ds2-5-button--secondary ds2-5-button--inverse"><span class="material-symbols-outlined" style="font-size: 20px" translate="no">close</span></button></div><div class="ds-signup-banner-ctas"><img src="//a.academia-assets.com/images/academia-logo-capital-white.svg" /><h4 class="ds2-5-heading-serif-sm">Sign up for access to the world's latest research</h4><button class="ds2-5-button ds2-5-button--inverse ds2-5-button--full-width js-swp-download-button" data-signup-modal="{"location":"signup-banner"}">Sign up for free<span class="material-symbols-outlined" style="font-size: 20px" translate="no">arrow_forward</span></button></div><div class="ds-signup-banner-divider"></div><div class="ds-signup-banner-reasons"><div class="ds-signup-banner-reasons-item"><span class="material-symbols-outlined" style="font-size: 24px" translate="no">check</span><span>Get notified about relevant papers</span></div><div class="ds-signup-banner-reasons-item"><span class="material-symbols-outlined" style="font-size: 24px" translate="no">check</span><span>Save papers to use in your research</span></div><div class="ds-signup-banner-reasons-item"><span class="material-symbols-outlined" style="font-size: 24px" translate="no">check</span><span>Join the discussion with peers</span></div><div class="ds-signup-banner-reasons-item"><span class="material-symbols-outlined" style="font-size: 24px" translate="no">check</span><span>Track your impact</span></div></div></div><script>(() => { // Set up signup banner show/hide behavior: // 1. 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The details of the structures connected to the central sources, such as the circumstellar discs and the morphology of the jets at their launching points, still lack of observational evidence. In this thesis, the high-mass star forming process is investigated in terms of the evolution of high-mass clumps selected from the ATLASGAL survey based on their 12 CO emission in the sub-millimetre. While single-dish sub-millimetre observations provide a large-scale view of the high-mass star formation process, higher angular resolution observations are required to disentangle the details of the protostars within the clumps. For this, threedimensional infrared spectroscopy was obtained for a group of RMS sources to characterise the circumstellar environment of high-mass YSOs in linear scales of ∼100-1000 AU. The ATLASGAL TOP100 sample offers a unique opportunity to analyse a statistically complete sample of high-mass clumps at different evolutionary stages. APEX data of three rotational J transitions of the CO (the CO (4-3), CO (6-5) and CO (7-6)) were used to characterise the properties of their warm gas (155 K) content and to derive the relations between the CO and the clump properties. The CO line luminosities were derived and the analysis indicated that the CO emission increases as a function of the evolutionary stage of the clumps (from infrared-weak to H ii regions) and as a function of the bolometric luminosity (L bol) and mass of the sources (M clump). The comparison of the TOP100 with low-mass objects observed in the CO (6-5) and CO (7-6), together with CO (10-9) data observed for a complementary sample of objects indicated that the dependency of the CO luminosity (L CO) with the bolometric luminosity of the sources gets steeper towards higher-J transitions. Although the CO luminosity of more luminous clumps are systematically larger than the values obtained for the less luminous sources, the individual analysis of each subsample suggests a similar dependency of L CO versus L bol for each luminosity regime. Finally, the presence of high-velocity CO emission observed for the TOP100 suggests that ∼85% of the sources are driving molecular outflows. The selection of isolated high-mass objects undergoing mass accretion is fundamental to investigate if these objects are formed through an accretion disc or if they are formed by merging of low-mass YSOs. The near-infrared window provides one of the best opportunities to investigate the interior of the sub-mm clumps and study in details their individual members. Thanks to the relatively high-resolution obtained in the K-band and the moderate reddening effectsin the K-band, a sample of eight (8) HMYSOs exhibiting large-scale H 2 outflows were selected to follow-up K-band spectroscopic observations using the NIFS spectrometer (Gemini North). All sources exhibit extended continuum emission and exhibit atomic and molecular transitions typical of embedded objects, such as Brγ, H 2 and the CO lines. The H 2 lines are tracing the launching point of the large-scale jets in scales of ∼ 100 AU in five of eight sources (63%). The identification of jets at such small scales indicates that these objects are still undergoing mass accretion. The Brγ emission probes the ionised gas around the HMYSOs. The analysis of the Brγ spectro-astrometry at sub-pixel scales suggests that the line arises from the cavity of the outflows or from rotating structures perpendicular to the H 2 jets (i.e., disc). Five sources also exhibit CO emission features (63%), and three HMYSOs display CO absorption features (38%), indicating that they are likely associated with circumstellar discs. By further investigating the kinematics of the spatially resolved CO absorption features, the Keplerian mass of three sources was estimated in 5±3, 8±5 and 30±10 M ⊙. These results support that high-mass stars are formed through discs, similarly as observed towards low-mass stars. The comparison between the collimation degree of the molecular jets or outflows detected in the NIFS data with their large-scale counterparts indicate that these structures present a relatively wide range of collimation degrees.</p><div class="ds-related-work--ctas"><button class="ds2-5-text-link ds2-5-text-link--inline js-swp-download-button" data-signup-modal="{"location":"wsj-grid-card-download-pdf-modal","work_title":"The Formation of High-Mass Stars: from High-Mass Clumps to Accretion Discs and Molecular Outflows","attachmentId":69478380,"attachmentType":"pdf","work_url":"https://www.academia.edu/52020961/The_Formation_of_High_Mass_Stars_from_High_Mass_Clumps_to_Accretion_Discs_and_Molecular_Outflows","alternativeTracking":true}"><span class="material-symbols-outlined" style="font-size: 18px" translate="no">download</span><span class="ds2-5-text-link__content">Download free PDF</span></button><a class="ds2-5-text-link ds2-5-text-link--inline js-wsj-grid-card-view-pdf" href="https://www.academia.edu/52020961/The_Formation_of_High_Mass_Stars_from_High_Mass_Clumps_to_Accretion_Discs_and_Molecular_Outflows"><span class="ds2-5-text-link__content">View PDF</span><span class="material-symbols-outlined" style="font-size: 18px" translate="no">chevron_right</span></a></div></div><div class="ds-related-work--container js-wsj-grid-card" data-collection-position="1" data-entity-id="86777454" data-sort-order="default"><a class="ds-related-work--title js-wsj-grid-card-title ds2-5-body-md ds2-5-body-link" href="https://www.academia.edu/86777454/Dense_Cores_Filaments_and_Outflows_in_the_S255IR_Region_of_High_mass_Star_Formation">Dense Cores, Filaments, and Outflows in the S255IR Region of High-mass Star Formation</a><div class="ds-related-work--metadata"><a class="js-wsj-grid-card-author ds2-5-body-sm ds2-5-body-link" data-author-id="52801245" href="https://ipfran.academia.edu/IgorZinchenko">Igor Zinchenko</a></div><p class="ds-related-work--metadata ds2-5-body-xs">The Astrophysical Journal, 2020</p><p class="ds-related-work--abstract ds2-5-body-sm">We investigate at a high angular resolution the spatial and kinematic structure of the S255IR high-mass starforming region, which demonstrated recently the first disk-mediated accretion burst in the massive young stellar object. The observations were performed with the Atacama Large Millimeter/submillimeter Array (ALMA) in Band 7 at an angular resolution of ∼ 0 1, which corresponds to ∼180au. The 0.9mm continuum, C 34 S(7-6) and CCH N=4−3 data show a presence of very narrow (∼1000 au), very dense (n ∼ 10 7 cm −3), and warm filamentary structures in this area. At least some of them represent apparently dense walls around the high velocity molecular outflow with a wide opening angle from the S255IR-SMA1 core, which is associated with the NIRS3 YSO. This wide-angle outflow surrounds a narrow jet. At the ends of the molecular outflow there are shocks, traced in the SiO(8-7) emission. The SiO abundance there is enhanced by at least 3 orders of magnitude. The CO(3-2) and SiO(8-7) data show a collimated and extended high velocity outflow from another dense core in this area, SMA2. The outflow is bent and consists of a chain of knots, which may indicate periodic ejections possibly arising from a binary system consisting of low-or intermediate-mass protostars. The C 34 S emission shows evidence of rotation of the parent core. Finally, we detected two new low-mass compact cores in this area (designated as SMM1 and SMM2), which may represent prestellar objects.</p><div class="ds-related-work--ctas"><button class="ds2-5-text-link ds2-5-text-link--inline js-swp-download-button" data-signup-modal="{"location":"wsj-grid-card-download-pdf-modal","work_title":"Dense Cores, Filaments, and Outflows in the S255IR Region of High-mass Star Formation","attachmentId":91155863,"attachmentType":"pdf","work_url":"https://www.academia.edu/86777454/Dense_Cores_Filaments_and_Outflows_in_the_S255IR_Region_of_High_mass_Star_Formation","alternativeTracking":true}"><span class="material-symbols-outlined" style="font-size: 18px" translate="no">download</span><span class="ds2-5-text-link__content">Download free PDF</span></button><a class="ds2-5-text-link ds2-5-text-link--inline js-wsj-grid-card-view-pdf" href="https://www.academia.edu/86777454/Dense_Cores_Filaments_and_Outflows_in_the_S255IR_Region_of_High_mass_Star_Formation"><span class="ds2-5-text-link__content">View PDF</span><span class="material-symbols-outlined" style="font-size: 18px" translate="no">chevron_right</span></a></div></div><div class="ds-related-work--container js-wsj-grid-card" data-collection-position="2" data-entity-id="113889069" data-sort-order="default"><a class="ds-related-work--title js-wsj-grid-card-title ds2-5-body-md ds2-5-body-link" href="https://www.academia.edu/113889069/ALMA_Reveals_Sequential_High_mass_Star_Formation_in_the_G9_62_0_19_Complex">ALMA Reveals Sequential High-mass Star Formation in the G9.62+0.19 Complex</a><div class="ds-related-work--metadata"><a class="js-wsj-grid-card-author ds2-5-body-sm ds2-5-body-link" data-author-id="6002801" href="https://uchile.academia.edu/DiegoMardones">Diego Mardones</a></div><p class="ds-related-work--metadata ds2-5-body-xs">The Astrophysical Journal, 2017</p><p class="ds-related-work--abstract ds2-5-body-sm">Stellar feedback from high-mass stars (e.g., H II regions) can strongly influence the surrounding interstellar medium and regulate star formation. Our new ALMA observations reveal sequential high-mass star formation taking place within one subvirial filamentary clump (the G9.62 clump) in the G9.62+0.19 complex. The 12 dense cores (MM1-MM12) detected by ALMA are at very different evolutionary stages, from the starless core phase to the UC H II region phase. Three dense cores (MM6, MM7/G, MM8/F) are associated with outflows. The massvelocity diagrams of the outflows associated with MM7/G and MM8/F can be well-fit by broken power laws. The mass-velocity diagram of the SiO outflow associated with MM8/F breaks much earlier than other outflow tracers (e.g., CO, SO, CS, HCN), suggesting that SiO traces newly shocked gas, while the other molecular lines (e.g., CO, SO, CS, HCN) mainly trace the ambient gas continuously entrained by outflow jets. Five cores (MM1, MM3, MM5, MM9, MM10) are massive starless core candidates whose masses are estimated to be larger than 25 M ☉ , assuming a dust temperature of 20 K. The shocks from the expanding H II regions ("B" and "C") to the west may have a great impact on the G9.62 clump by compressing it into a filament and inducing core collapse successively, leading to sequential star formation. Our findings suggest that stellar feedback from H II regions may enhance the star formation efficiency and suppress low-mass star formation in adjacent pre-existing massive clumps.</p><div class="ds-related-work--ctas"><button class="ds2-5-text-link ds2-5-text-link--inline js-swp-download-button" data-signup-modal="{"location":"wsj-grid-card-download-pdf-modal","work_title":"ALMA Reveals Sequential High-mass Star Formation in the G9.62+0.19 Complex","attachmentId":110733420,"attachmentType":"pdf","work_url":"https://www.academia.edu/113889069/ALMA_Reveals_Sequential_High_mass_Star_Formation_in_the_G9_62_0_19_Complex","alternativeTracking":true}"><span class="material-symbols-outlined" style="font-size: 18px" translate="no">download</span><span class="ds2-5-text-link__content">Download free PDF</span></button><a class="ds2-5-text-link ds2-5-text-link--inline js-wsj-grid-card-view-pdf" href="https://www.academia.edu/113889069/ALMA_Reveals_Sequential_High_mass_Star_Formation_in_the_G9_62_0_19_Complex"><span class="ds2-5-text-link__content">View PDF</span><span class="material-symbols-outlined" style="font-size: 18px" translate="no">chevron_right</span></a></div></div><div class="ds-related-work--container js-wsj-grid-card" data-collection-position="3" data-entity-id="107426806" data-sort-order="default"><a class="ds-related-work--title js-wsj-grid-card-title ds2-5-body-md ds2-5-body-link" href="https://www.academia.edu/107426806/Unifying_low_and_high_mass_star_formation_through_density_amplified_hubs_of_filaments">Unifying low- and high-mass star formation through density-amplified hubs of filaments</a><div class="ds-related-work--metadata"><a class="js-wsj-grid-card-author ds2-5-body-sm ds2-5-body-link" data-author-id="41285986" href="https://nagoya-u.academia.edu/ShuichiroInutsuka">Shu-ichiro Inutsuka</a></div><p class="ds-related-work--metadata ds2-5-body-xs">Astronomy and Astrophysics, 2020</p><p class="ds-related-work--abstract ds2-5-body-sm">Context. Star formation takes place in giant molecular clouds, resulting in mass-segregated young stellar clusters composed of Sunlike stars, brown dwarfs, and massive O-type(50-100 M) stars. Aims. We aim to identify candidate hub-filament systems (HFSs) in the Milky Way and examine their role in the formation of the highest mass stars and star clusters. Methods. The Herschel survey HiGAL has catalogued about 10 5 clumps. Of these, approximately 35 000 targets are detected at the 3σ level in a minimum of four bands. Using the DisPerSE algorithm we detect filamentary skeletons on 10 × 10 cutouts of the SPIRE 250 µm images (18 beam width) of the targets. Any filament with a total length of at least 55 (3 × 18) and at least 18 inside the clump was considered to form a junction at the clump. A hub is defined as a junction of three or more filaments. Column density maps were masked by the filament skeletons and averaged for HFS and non-HFS samples to compute the radial profile along the filaments into the clumps. Results. Approximately 3700 (11%) are candidate HFSs, of which about 2150 (60%) are pre-stellar and 1400 (40%) are protostellar. The filaments constituting the HFSs have a mean length of ∼10-20 pc, a mass of ∼5 × 10 4 M , and line masses (M/L) of ∼2 × 10 3 M pc −1. All clumps with L > 10 4 L and L > 10 5 L at distances within 2 and 5 kpc respectively are located in the hubs of HFSs. The column densities of hubs are found to be enhanced by a factor of approximately two (pre-stellar sources) up to about ten (proto-stellar sources). Conclusions. All high-mass stars preferentially form in the density-enhanced hubs of HFSs. This amplification can drive the observed longitudinal flows along filaments providing further mass accretion. Radiation pressure and feedback can escape into the interfilamentary voids. We propose a "filaments to clusters" unified paradigm for star formation, with the following salient features: (a) low-intermediate-mass stars form slowly (10 6 yr) in the filaments and massive stars form quickly (10 5 yr) in the hub, (b) the initial mass function is the sum of stars continuously created in the HFS with all massive stars formed in the hub, (c) feedback dissipation and mass segregation arise naturally due to HFS properties, and explain the (d) age spreads within bound clusters and the formation of isolated OB associations.</p><div class="ds-related-work--ctas"><button class="ds2-5-text-link ds2-5-text-link--inline js-swp-download-button" data-signup-modal="{"location":"wsj-grid-card-download-pdf-modal","work_title":"Unifying low- and high-mass star formation through density-amplified hubs of filaments","attachmentId":106096076,"attachmentType":"pdf","work_url":"https://www.academia.edu/107426806/Unifying_low_and_high_mass_star_formation_through_density_amplified_hubs_of_filaments","alternativeTracking":true}"><span class="material-symbols-outlined" style="font-size: 18px" translate="no">download</span><span class="ds2-5-text-link__content">Download free PDF</span></button><a class="ds2-5-text-link ds2-5-text-link--inline js-wsj-grid-card-view-pdf" href="https://www.academia.edu/107426806/Unifying_low_and_high_mass_star_formation_through_density_amplified_hubs_of_filaments"><span class="ds2-5-text-link__content">View PDF</span><span class="material-symbols-outlined" style="font-size: 18px" translate="no">chevron_right</span></a></div></div><div class="ds-related-work--container js-wsj-grid-card" data-collection-position="4" data-entity-id="26196324" data-sort-order="default"><a class="ds-related-work--title js-wsj-grid-card-title ds2-5-body-md ds2-5-body-link" href="https://www.academia.edu/26196324/G30_79_FIR_10_a_gravitationally_bound_infalling_high_mass_star_forming_clump">G30.79 FIR 10: a gravitationally bound infalling high-mass star-forming clump</a><div class="ds-related-work--metadata"><a class="js-wsj-grid-card-author ds2-5-body-sm ds2-5-body-link" data-author-id="41802335" href="https://nrao.academia.edu/EduardoHardy">Eduardo Hardy</a></div><p class="ds-related-work--metadata ds2-5-body-xs">Astronomy and Astrophysics, 2010</p><p class="ds-related-work--abstract ds2-5-body-sm">Context. The process of high-mass star formation is still shrouded in controversy. Models are still tentative and current observations are just beginning to probe the densest inner regions of giant molecular clouds. Aims. The study of high-mass star formation requires the observation and analysis of high density gas. This can be achieved by the detection of emission from higher rotational transitions of molecules in the sub-millimeter. Here, we studied the high-mass clump G30.79 FIR 10 by observing molecular emission in the 345 GHz band. The goal is to understand the gravitational state of this clump, considering turbulence and magnetic fields, and to study the kinematics of dense gas. Methods. We approached this region by mapping the spatial distribution of HCO + (J = 4 → 3), H 13 CO + (J = 4 → 3), CS(J = 7 → 6), 12 CO(J = 3 → 2), and 13 CO(J = 3 → 2) molecular emission by using the ASTE telescope and by observing the 12 C 18 O(J = 3 → 2), HCN(J = 4 → 3), and H 13 CN(J = 4 → 3) molecular transitions with the APEX telescope. Results. Infalling motions were detected and modeled toward this source. A mean infall velocity of 0.5 km s −1 with an infall mass rate of 5 × 10 −3 M ⊙ /yr was obtained. Also, a previously estimated value for the magnetic field strength in the plane of the sky was refined to be 855 µG which we used to calculate a mass-to-magnetic flux ratio, λ = 1.9, or super-critical. The virial mass from turbulent motions was also calculated finding M vir = 563 M ⊙ , which gives a ratio of M submm /M vir =5.9. Both values strongly suggest that this clump must be in a state of gravitational collapse. Additionally, we estimated the HCO + abundance, obtaining X(HCO + )= 2.4×10 −10 .</p><div class="ds-related-work--ctas"><button class="ds2-5-text-link ds2-5-text-link--inline js-swp-download-button" data-signup-modal="{"location":"wsj-grid-card-download-pdf-modal","work_title":"G30.79 FIR 10: a gravitationally bound infalling high-mass star-forming clump","attachmentId":46517701,"attachmentType":"pdf","work_url":"https://www.academia.edu/26196324/G30_79_FIR_10_a_gravitationally_bound_infalling_high_mass_star_forming_clump","alternativeTracking":true}"><span class="material-symbols-outlined" style="font-size: 18px" translate="no">download</span><span class="ds2-5-text-link__content">Download free PDF</span></button><a class="ds2-5-text-link ds2-5-text-link--inline js-wsj-grid-card-view-pdf" href="https://www.academia.edu/26196324/G30_79_FIR_10_a_gravitationally_bound_infalling_high_mass_star_forming_clump"><span class="ds2-5-text-link__content">View PDF</span><span class="material-symbols-outlined" style="font-size: 18px" translate="no">chevron_right</span></a></div></div><div class="ds-related-work--container js-wsj-grid-card" data-collection-position="5" data-entity-id="6199763" data-sort-order="default"><a class="ds-related-work--title js-wsj-grid-card-title ds2-5-body-md ds2-5-body-link" href="https://www.academia.edu/6199763/Star_Forming_Cores_Embedded_in_a_Massive_Cold_Clump_Fragmentation_Collapse_and_Energetic_Outflows">Star-Forming Cores Embedded in a Massive Cold Clump: Fragmentation, Collapse, and Energetic Outflows</a><div class="ds-related-work--metadata"><a class="js-wsj-grid-card-author ds2-5-body-sm ds2-5-body-link" data-author-id="21835" href="https://esa.academia.edu/StephanBirkmann">Stephan Birkmann</a></div><p class="ds-related-work--metadata ds2-5-body-xs">Astrophysical Journal, 2009</p><p class="ds-related-work--abstract ds2-5-body-sm">The fate of massive cold clumps, their internal structure and collapse need to be characterised to understand the initial conditions for the formation of high-mass stars, stellar systems, and the origin of associations and clusters. We explore the onset of star formation in the 75 M_sun SMM1 clump in the region ISOSS J18364-0221 using infrared and (sub-)millimetre observations including interferometry. This contracting clump has fragmented into two compact cores SMM1 North and South of 0.05 pc radius, having masses of 15 and 10 M_sun, and luminosities of 20 and 180 L_sun. SMM1 South harbours a source traced at 24 and 70um, drives an energetic molecular outflow, and appears supersonically turbulent at the core centre. SMM1 North has no infrared counterparts and shows lower levels of turbulence, but also drives an outflow. Both outflows appear collimated and parsec-scale near-infrared features probably trace the outflow-powering jets. We derived mass outflow rates of at least 4E-5 M_sun/yr and outflow timescales of less than 1E4 yr. Our HCN(1-0) modelling for SMM1 South yielded an infall velocity of 0.14 km/s and an estimated mass infall rate of 3E-5 M_sun/yr. Both cores may harbour seeds of intermediate- or high-mass stars. We compare the derived core properties with recent simulations of massive core collapse. They are consistent with the very early stages dominated by accretion luminosity.</p><div class="ds-related-work--ctas"><button class="ds2-5-text-link ds2-5-text-link--inline js-swp-download-button" data-signup-modal="{"location":"wsj-grid-card-download-pdf-modal","work_title":"Star-Forming Cores Embedded in a Massive Cold Clump: Fragmentation, Collapse, and Energetic Outflows","attachmentId":33076111,"attachmentType":"pdf","work_url":"https://www.academia.edu/6199763/Star_Forming_Cores_Embedded_in_a_Massive_Cold_Clump_Fragmentation_Collapse_and_Energetic_Outflows","alternativeTracking":true}"><span class="material-symbols-outlined" style="font-size: 18px" translate="no">download</span><span class="ds2-5-text-link__content">Download free PDF</span></button><a class="ds2-5-text-link ds2-5-text-link--inline js-wsj-grid-card-view-pdf" href="https://www.academia.edu/6199763/Star_Forming_Cores_Embedded_in_a_Massive_Cold_Clump_Fragmentation_Collapse_and_Energetic_Outflows"><span class="ds2-5-text-link__content">View PDF</span><span class="material-symbols-outlined" style="font-size: 18px" translate="no">chevron_right</span></a></div></div><div class="ds-related-work--container js-wsj-grid-card" data-collection-position="6" data-entity-id="117866187" data-sort-order="default"><a class="ds-related-work--title js-wsj-grid-card-title ds2-5-body-md ds2-5-body-link" href="https://www.academia.edu/117866187/Dense_Molecular_Clumps_Associated_with_Young_Clusters_in_Massive_Star_forming_Regions">Dense Molecular Clumps Associated with Young Clusters in Massive Star‐forming Regions</a><div class="ds-related-work--metadata"><a class="js-wsj-grid-card-author ds2-5-body-sm ds2-5-body-link" data-author-id="305298372" href="https://naoj.academia.edu/KazuyoshiSunada">Kazuyoshi Sunada</a></div><p class="ds-related-work--metadata ds2-5-body-xs">The Astrophysical Journal, 2007</p><p class="ds-related-work--abstract ds2-5-body-sm">We present the results of C 18 O observations by the 45 m Nobeyama radio telescope toward dense clumps with young clusters in nine massive star-forming regions. We identified 39 clumps whose mass, radius, and line width range from 15 to 1500 M , from 0.14 to 0.76 pc, and from 0.6 to 3.2 km s À1 , respectively. The clumps associated with massive (proto)stars have a large line width ($2.5 km s À1) and a large mass ($500 M). Most of the clumps are sufficiently gravitationally bound because they have a virial mass similar to the gas mass, and the average H 2 density of the clumps increases with increasing internal kinetic motion. Next, we found two relations, one between the number density of associated 2MASS sources and the average H 2 density of the clump and the other between the number density of sources and the star formation efficiency of the clump. From these results, we suggest that a structure, whose size scale is $0.3 pc, with a high average H 2 density is required in order for cluster formation to occur. In addition, we found that the internal kinetic motion of a clump has to be large in order to form massive stars, because there is a good correlation between the maximum mass of associated stars and the line width of the clump. Such clumps with large internal motion must generally have a high average H 2 density in order to be gravitationally bound. Thus, massive stars are formed in a dense cluster.</p><div class="ds-related-work--ctas"><button class="ds2-5-text-link ds2-5-text-link--inline js-swp-download-button" data-signup-modal="{"location":"wsj-grid-card-download-pdf-modal","work_title":"Dense Molecular Clumps Associated with Young Clusters in Massive Star‐forming Regions","attachmentId":113619154,"attachmentType":"pdf","work_url":"https://www.academia.edu/117866187/Dense_Molecular_Clumps_Associated_with_Young_Clusters_in_Massive_Star_forming_Regions","alternativeTracking":true}"><span class="material-symbols-outlined" style="font-size: 18px" translate="no">download</span><span class="ds2-5-text-link__content">Download free PDF</span></button><a class="ds2-5-text-link ds2-5-text-link--inline js-wsj-grid-card-view-pdf" href="https://www.academia.edu/117866187/Dense_Molecular_Clumps_Associated_with_Young_Clusters_in_Massive_Star_forming_Regions"><span class="ds2-5-text-link__content">View PDF</span><span class="material-symbols-outlined" style="font-size: 18px" translate="no">chevron_right</span></a></div></div><div class="ds-related-work--container js-wsj-grid-card" data-collection-position="7" data-entity-id="56029621" data-sort-order="default"><a class="ds-related-work--title js-wsj-grid-card-title ds2-5-body-md ds2-5-body-link" href="https://www.academia.edu/56029621/Filaments_Collapse_and_Outflows_in_Massive_Star_Formation">Filaments, Collapse and Outflows in Massive Star Formation</a><div class="ds-related-work--metadata"><a class="js-wsj-grid-card-author ds2-5-body-sm ds2-5-body-link" data-author-id="33292566" href="https://independent.academia.edu/RalphPudritz">Ralph Pudritz</a></div><p class="ds-related-work--abstract ds2-5-body-sm">We present results from our numerical simulations of collapsing massive molecular cloud cores. These numerical calculations show that massive stars assemble quickly with mass accretion rates exceeding 10 −3 M ⊙ yr −1 and confirm that the mass accretion during the collapsing phase is much more efficient than predicted by selfsimilar collapse solutions,Ṁ ∼ c 3 /G. We find that during protostellar assembly out of a non-turbulent core, the mass accretion reaches 20 − 100c 3 /G. Furthermore, we explore the self-consistent structure of bipolar outflows that are produced in our three dimensional magnetized collapse simulations. These outflows produce cavities out of which radiation pressure can be released, thereby reducing the limitations on the final mass of massive stars formed by gravitational collapse. Additional enhancement of the mass accretion rate comes from accretion along filaments that are built up by supersonic turbulent motions. Our numerical calculations of collapsing turbulent cores result in mass accretion rates as high as 10 −2 M ⊙ yr −1 .</p><div class="ds-related-work--ctas"><button class="ds2-5-text-link ds2-5-text-link--inline js-swp-download-button" data-signup-modal="{"location":"wsj-grid-card-download-pdf-modal","work_title":"Filaments, Collapse and Outflows in Massive Star Formation","attachmentId":71616559,"attachmentType":"pdf","work_url":"https://www.academia.edu/56029621/Filaments_Collapse_and_Outflows_in_Massive_Star_Formation","alternativeTracking":true}"><span class="material-symbols-outlined" style="font-size: 18px" translate="no">download</span><span class="ds2-5-text-link__content">Download free PDF</span></button><a class="ds2-5-text-link ds2-5-text-link--inline js-wsj-grid-card-view-pdf" href="https://www.academia.edu/56029621/Filaments_Collapse_and_Outflows_in_Massive_Star_Formation"><span class="ds2-5-text-link__content">View PDF</span><span class="material-symbols-outlined" style="font-size: 18px" translate="no">chevron_right</span></a></div></div><div class="ds-related-work--container js-wsj-grid-card" data-collection-position="8" data-entity-id="113961180" data-sort-order="default"><a class="ds-related-work--title js-wsj-grid-card-title ds2-5-body-md ds2-5-body-link" href="https://www.academia.edu/113961180/The_Formation_of_Massive_Stars">The Formation of Massive Stars</a><div class="ds-related-work--metadata"><a class="js-wsj-grid-card-author ds2-5-body-sm ds2-5-body-link" data-author-id="71144612" href="https://independent.academia.edu/janPalous">jan Palous</a></div><p class="ds-related-work--metadata ds2-5-body-xs">Astronomische Nachrichten, 2004</p><p class="ds-related-work--abstract ds2-5-body-sm">We present a model for the formation of massive (M > ∼ 10M ⊙) stars through accretioninduced collisions in the cores of embedded dense stellar clusters. This model circumvents the problem of accreting onto a star whose luminosity is sufficient to reverse the infall of gas. Instead, the central core of the cluster accretes from the surrounding gas, thereby decreasing its radius until collisions between individual components become significant. These components are, in general, intermediate-mass stars that have formed through accretion onto low-mass protostars. Once a sufficiently massive star has formed to expel the remaining gas, the cluster expands in accordance with this loss of mass, halting further collisions. This process implies a critical stellar density for the formation of massive stars, and a high rate of binaries formed by tidal capture.</p><div class="ds-related-work--ctas"><button class="ds2-5-text-link ds2-5-text-link--inline js-swp-download-button" data-signup-modal="{"location":"wsj-grid-card-download-pdf-modal","work_title":"The Formation of Massive Stars","attachmentId":110786210,"attachmentType":"pdf","work_url":"https://www.academia.edu/113961180/The_Formation_of_Massive_Stars","alternativeTracking":true}"><span class="material-symbols-outlined" style="font-size: 18px" translate="no">download</span><span class="ds2-5-text-link__content">Download free PDF</span></button><a class="ds2-5-text-link ds2-5-text-link--inline js-wsj-grid-card-view-pdf" href="https://www.academia.edu/113961180/The_Formation_of_Massive_Stars"><span class="ds2-5-text-link__content">View PDF</span><span class="material-symbols-outlined" style="font-size: 18px" translate="no">chevron_right</span></a></div></div><div class="ds-related-work--container js-wsj-grid-card" data-collection-position="9" data-entity-id="53050507" data-sort-order="default"><a class="ds-related-work--title js-wsj-grid-card-title ds2-5-body-md ds2-5-body-link" href="https://www.academia.edu/53050507/High_Resolution_Studies_of_the_Multiple_Core_Systems_toward_Cluster_forming_Regions_Including_Massive_Stars">High‐Resolution Studies of the Multiple‐Core Systems toward Cluster‐forming Regions Including Massive Stars</a><div class="ds-related-work--metadata"><a class="js-wsj-grid-card-author ds2-5-body-sm ds2-5-body-link" data-author-id="57155228" href="https://independent.academia.edu/YoshinoriYonekura">Yoshinori Yonekura</a></div><p class="ds-related-work--metadata ds2-5-body-xs">The Astrophysical Journal Supplement Series, 2008</p><p class="ds-related-work--abstract ds2-5-body-sm">We present the results of C 18 O observations by the Nobeyama Millimeter Array toward dense clumps with radii of ∼ 0.3 pc in six cluster-forming regions including massive (proto)stars. We identified 171 cores, whose radius, line width, and molecular mass range from 0.01 to 0.09 pc, 0.43 to 3.33 km s −1 , and 0.5 to 54.1 M ⊙ , respectively. Many cores with various line widths exist in one clump, and the index of the line width-radius relationship of the cores and the parental clump differs from core to core in the clump. This indicates that the degree of dissipation of the turbulent motion varies for each core in one clump. Although the mass of the cores increases with the line width, most cores are gravitationally bound by the external pressure. In addition, the line width and the external pressure of the cores tend to decrease with the distance from the center of the clump, and these dependencies may be caused by the inner H 2 density structure of the clump that affects the physical properties of the cores. Moreover, the number density of the cores and the number density of young (proto)stars have a similar relationship to the average H 2 density of the clumps. Thus, our findings suggest that the cluster is formed in the clump through the formation of such multiple cores, whose physical properties would have been strongly related to the H 2 density structure and the turbulent motion of the clump.</p><div class="ds-related-work--ctas"><button class="ds2-5-text-link ds2-5-text-link--inline js-swp-download-button" data-signup-modal="{"location":"wsj-grid-card-download-pdf-modal","work_title":"High‐Resolution Studies of the Multiple‐Core Systems toward Cluster‐forming Regions Including Massive Stars","attachmentId":70016895,"attachmentType":"pdf","work_url":"https://www.academia.edu/53050507/High_Resolution_Studies_of_the_Multiple_Core_Systems_toward_Cluster_forming_Regions_Including_Massive_Stars","alternativeTracking":true}"><span class="material-symbols-outlined" style="font-size: 18px" translate="no">download</span><span class="ds2-5-text-link__content">Download free PDF</span></button><a class="ds2-5-text-link ds2-5-text-link--inline js-wsj-grid-card-view-pdf" href="https://www.academia.edu/53050507/High_Resolution_Studies_of_the_Multiple_Core_Systems_toward_Cluster_forming_Regions_Including_Massive_Stars"><span class="ds2-5-text-link__content">View PDF</span><span class="material-symbols-outlined" style="font-size: 18px" translate="no">chevron_right</span></a></div></div></div></div><div class="ds-sticky-ctas--wrapper js-loswp-sticky-ctas hidden"><div class="ds-sticky-ctas--grid-container"><div class="ds-sticky-ctas--container"><button class="ds2-5-button js-swp-download-button" data-signup-modal="{"location":"continue-reading-button--sticky-ctas","attachmentId":55404248,"attachmentType":"pdf","workUrl":null}">See full PDF</button><button class="ds2-5-button ds2-5-button--secondary js-swp-download-button" data-signup-modal="{"location":"download-pdf-button--sticky-ctas","attachmentId":55404248,"attachmentType":"pdf","workUrl":null}"><span class="material-symbols-outlined" style="font-size: 20px" translate="no">download</span>Download PDF</button></div></div></div><div class="ds-below-fold--grid-container"><div class="ds-work--container js-loswp-embedded-document"><div class="attachment_preview" data-attachment="Attachment_55404248" style="display: none"><div class="js-scribd-document-container"><div class="scribd--document-loading js-scribd-document-loader" style="display: block;"><img alt="Loading..." src="//a.academia-assets.com/images/loaders/paper-load.gif" /><p>Loading Preview</p></div></div><div style="text-align: center;"><div class="scribd--no-preview-alert js-preview-unavailable"><p>Sorry, preview is currently unavailable. 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