{"id":4226,"date":"2018-01-11T00:31:04","date_gmt":"2018-01-10T20:31:04","guid":{"rendered":"http:\/\/sites.williams.edu\/kkwitter\/?page_id=4226"},"modified":"2018-04-12T18:44:34","modified_gmt":"2018-04-12T14:44:34","slug":"a402t-tutorial-week-7-nebular-diagnostics","status":"publish","type":"page","link":"https:\/\/sites.williams.edu\/kkwitter\/astronomy-402-between-the-stars\/a402t-tutorial-week-7-nebular-diagnostics\/","title":{"rendered":"A402T Tutorial Week #7: Nebular Diagnostics"},"content":{"rendered":"<p><strong>ASTRONOMY 402T \u2013 Spring 2018<br \/>\nProblems for Tutorial Week #7<\/strong><\/p>\n<p><strong>PART A<\/strong><\/p>\n<p><strong>1<\/strong>. a) Explain in detail why the intensity ratios of density-indicating pairs like [S II] \u03bb\u03bb6717\/6731 and [O II] \u03bb\u03bb3729\/3726, in fact\u00a0<strong><em>do<\/em><\/strong> allow us to calculate the nebular density.<\/p>\n<p>b) Consider the density-indicating pairs [O II] \u03bb\u03bb3729\/3726 and [Ar IV] \u03bb\u03bb4711\/4740. Draw and label their energy level diagrams. In what density regimes are the [O II] and the [Ar IV] pairs useful?<\/p>\n<p>c) Why <em><strong>is<\/strong><\/em>\u00a0there a particular density regime for each pair, and what determines these regimes?<\/p>\n<p><strong>2. \u00a0<\/strong>Explain in detail why the intensity ratios of temperature-indicating pairs like [O III] \u03bb\u03bb4363\/5007 and [N II] \u03bb\u03bb5755\/6584, in fact\u00a0<strong><em>do<\/em><\/strong> allow us to calculate the temperature. Draw and label their energy level diagram.<\/p>\n<p><strong>3.\u00a0<\/strong>Discuss the ranges of temperature and density on H II regions and in planetary nebulae. How do they compare, and why?<\/p>\n<p><strong>PART B<\/strong><\/p>\n<p><strong>Do the PN Gallery <em>\u201cDetermining the Gas Density in Planetary Nebulae\u201d <\/em>exercise: <\/strong><\/p>\n<p><strong><a href=\"http:\/\/web.williams.edu\/Astronomy\/research\/PN\/nebulae\/exercise3.php\">http:\/\/web.williams.edu\/Astronomy\/research\/PN\/nebulae\/exercise3.php<\/a><\/strong><\/p>\n<p><strong>\u00a0<\/strong><\/p>\n","protected":false},"excerpt":{"rendered":"<p>ASTRONOMY 402T \u2013 Spring 2018 Problems for Tutorial Week #7 PART A 1. a) Explain in detail why the intensity ratios of density-indicating pairs like [S II] \u03bb\u03bb6717\/6731 and [O II] \u03bb\u03bb3729\/3726, in fact\u00a0do allow us to calculate the nebular density. b) Consider the density-indicating pairs [O II] \u03bb\u03bb3729\/3726 and [Ar IV] \u03bb\u03bb4711\/4740. Draw and [&hellip;]<\/p>\n","protected":false},"author":198,"featured_media":0,"parent":793,"menu_order":0,"comment_status":"closed","ping_status":"closed","template":"","meta":{"_acf_changed":false,"footnotes":""},"class_list":["post-4226","page","type-page","status-publish","hentry"],"acf":[],"_links":{"self":[{"href":"https:\/\/sites.williams.edu\/kkwitter\/wp-json\/wp\/v2\/pages\/4226","targetHints":{"allow":["GET"]}}],"collection":[{"href":"https:\/\/sites.williams.edu\/kkwitter\/wp-json\/wp\/v2\/pages"}],"about":[{"href":"https:\/\/sites.williams.edu\/kkwitter\/wp-json\/wp\/v2\/types\/page"}],"author":[{"embeddable":true,"href":"https:\/\/sites.williams.edu\/kkwitter\/wp-json\/wp\/v2\/users\/198"}],"replies":[{"embeddable":true,"href":"https:\/\/sites.williams.edu\/kkwitter\/wp-json\/wp\/v2\/comments?post=4226"}],"version-history":[{"count":13,"href":"https:\/\/sites.williams.edu\/kkwitter\/wp-json\/wp\/v2\/pages\/4226\/revisions"}],"predecessor-version":[{"id":4440,"href":"https:\/\/sites.williams.edu\/kkwitter\/wp-json\/wp\/v2\/pages\/4226\/revisions\/4440"}],"up":[{"embeddable":true,"href":"https:\/\/sites.williams.edu\/kkwitter\/wp-json\/wp\/v2\/pages\/793"}],"wp:attachment":[{"href":"https:\/\/sites.williams.edu\/kkwitter\/wp-json\/wp\/v2\/media?parent=4226"}],"curies":[{"name":"wp","href":"https:\/\/api.w.org\/{rel}","templated":true}]}}