{"id":66,"date":"2022-06-25T13:04:37","date_gmt":"2022-06-25T13:04:37","guid":{"rendered":"https:\/\/teams.issibern.ch\/turbulencesolarcorona\/?page_id=66"},"modified":"2022-06-25T13:20:12","modified_gmt":"2022-06-25T13:20:12","slug":"project-workplan","status":"publish","type":"page","link":"https:\/\/teams.issibern.ch\/turbulencesolarcorona\/project-description\/project-workplan\/","title":{"rendered":"Project Workplan"},"content":{"rendered":"

\u00a0 \u00a0 \u00a0 The work plan for the proposed meetings is the following: In the first task<\/strong>, the invited team
\nmembers that authored the different theoretical models of the solar wind will present observables
\nthat their theory predicts, and that can be compared to data obtained by the Parker Solar Probe. The
\nteam members were carefully selected in order to have a full representation of the different schools
\nof thought and approaches to theoretical solar wind modelling. The incompressible and reduced-
\nMHD models are presented by Dr. Asgari-Targhi and Dr. Verdini, the nearly incompressible model is
\npresented by Dr. Laxman, the compressible model based on the parametric decay is presented by Dr.
\nShoda, and the inhomogeneous compressible models are presented by Dr. Van Doorsselaere, Prof.
\nHillier, and Dr. Magyar. The related works are cited throughout the scientific rationale. In
\nparallel, team members specialized in observational analysis (Dr. Bandyopadhyay, Dr. Chen, Dr.
\nD\u2019Amicis, and Dr. Szabo) will present the latest results of the in-situ measurements in the solar wind.
\nSpecific scientific objectives<\/strong> are the determination of the properties of solar wind turbulence near
\nthe critical Alfv\u00e9n point and establishing whether these properties are different from those found in
\nthe sub- and super-Alfv\u00e9nic wind, based on Parker Solar Probe in-situ data. These properties of the
\nsolar wind are the perpendicular and parallel magnetic field, velocity, density, and energy spectra,
\nmagnitudes of Els\u00e4sser variables, cross-helicity, Alfv\u00e9nicity, compressibility.<\/p>\n

In the second task<\/strong>, similarities between theoretical predictions and measurements will be
\ndiscussed in open discussion session. Additionally, derived quantities that can be compared between
\ntheoretical models and observations will be proposed, in an iterative, refining process. These derived
\nquantities might include different statistical correlations between velocity, magnetic field, Els\u00e4sser
\nvariable perturbations and total magnetic field, background density, Alfv\u00e9n speed values and
\ngradients, nonlinear advective terms, etc. Specific scientific objectives<\/strong> are determining which
\ntheoretical models (incompressible, nearly-incompressible, compressible) explain best the
\nobservables established in the first task, and the calculation of the derived quantities and their
\ncomparison between theoretical models and observed values.<\/p>\n

In the third task<\/strong>, observational evidence that cannot be explained by the available models will be
\ndiscussed, along the required physics that is missing from the present models but might explain the
\nexperimental findings. Specific scientific objectives<\/strong> are the determination of properties of the solar
\nwind turbulence that are currently not explained by any of the presented models, and the
\nidentification of physical phenomena that might explain these properties.<\/p>\n

In the fourth task<\/strong>, the team will lay the foundations for the development of new, refined
\ntheoretical models of the solar corona and solar wind based on wave turbulence, that could explain
\nthe yet unexplained properties of the solar wind, determined in the third task. Specific scientific<\/strong>
\nobjectives<\/strong> are the determination of the details of analytical and\/or numerical models for an updated
\nsolar coronal and solar wind model, including the required physics, methods, and analysis, and
\ndevising a work plan for carrying out the construction of the model.<\/p>\n

Below you will find a schematic representation of the proposed project workplan:<\/p>\n

\"\"<\/p>\n","protected":false},"excerpt":{"rendered":"

\u00a0 \u00a0 \u00a0 The work plan for the proposed meetings is the following: In the first task, the invited team members that authored the different theoretical models of the solar wind will present observables that their theory predicts, and that can be compared to data obtained by the Parker Solar Probe. The team members were […]<\/p>\n","protected":false},"author":46,"featured_media":0,"parent":73,"menu_order":2,"comment_status":"closed","ping_status":"closed","template":"","meta":{"footnotes":""},"class_list":["post-66","page","type-page","status-publish","hentry"],"_links":{"self":[{"href":"https:\/\/teams.issibern.ch\/turbulencesolarcorona\/wp-json\/wp\/v2\/pages\/66","targetHints":{"allow":["GET"]}}],"collection":[{"href":"https:\/\/teams.issibern.ch\/turbulencesolarcorona\/wp-json\/wp\/v2\/pages"}],"about":[{"href":"https:\/\/teams.issibern.ch\/turbulencesolarcorona\/wp-json\/wp\/v2\/types\/page"}],"author":[{"embeddable":true,"href":"https:\/\/teams.issibern.ch\/turbulencesolarcorona\/wp-json\/wp\/v2\/users\/46"}],"replies":[{"embeddable":true,"href":"https:\/\/teams.issibern.ch\/turbulencesolarcorona\/wp-json\/wp\/v2\/comments?post=66"}],"version-history":[{"count":3,"href":"https:\/\/teams.issibern.ch\/turbulencesolarcorona\/wp-json\/wp\/v2\/pages\/66\/revisions"}],"predecessor-version":[{"id":70,"href":"https:\/\/teams.issibern.ch\/turbulencesolarcorona\/wp-json\/wp\/v2\/pages\/66\/revisions\/70"}],"up":[{"embeddable":true,"href":"https:\/\/teams.issibern.ch\/turbulencesolarcorona\/wp-json\/wp\/v2\/pages\/73"}],"wp:attachment":[{"href":"https:\/\/teams.issibern.ch\/turbulencesolarcorona\/wp-json\/wp\/v2\/media?parent=66"}],"curies":[{"name":"wp","href":"https:\/\/api.w.org\/{rel}","templated":true}]}}