Difference between revisions of "Talk:CG4 Proposal"
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And what is the importance of Young Stars, anyway? On the local scale, even small stars usually form discs, which often coalesce into planets. And some may be Earth-Like planets! On a more grand scale, formation and evolution of different types of stars, changes gas and dust and chemical composition of Galaxies; Evolution of the structural components of the universe, i.e. Galaxies, causes evolution of the Universe! | And what is the importance of Young Stars, anyway? On the local scale, even small stars usually form discs, which often coalesce into planets. And some may be Earth-Like planets! On a more grand scale, formation and evolution of different types of stars, changes gas and dust and chemical composition of Galaxies; Evolution of the structural components of the universe, i.e. Galaxies, causes evolution of the Universe! | ||
| − | We choose the Cometary Globules CG4 (R. A. 7 degrees 34’ 9”, Dec -56 degrees, Ecliptic Co-ords.) in which to look for new stars. The following is a summary of info describing the CG4- Gum Nebula environment, chosen because the area is visually and photometrically dense with star-forming material. (Used USNO http://www.nofs.navy.mil/data/fchPix to determine opacity of nebula and optical magnitude.) Through our collaborator J.S. Kim (U. AZ.) we have access to CG4 optical data in BVRI filters from the CTIO 0.9m.Extrapolating from this info may permit us to predict where and why new stars form. Conditional on the outcome of the first research step; The second step in our research is to determine whether a Cluster of New Stars exists in the area, and that information may to relevant to the study of Triggered Star Formation.(See “Spitzer Observations of IC 2118.) | + | We choose the Cometary Globules CG4 (R. A. 7 degrees 34’ 9”, Dec -56 degrees, Ecliptic Co-ords.) in which to look for new stars. The following is a summary of info describing the CG4- Gum Nebula environment, chosen because the area is visually and photometrically dense with star-forming material. (Used USNO http://www.nofs.navy.mil/data/fchPix to determine opacity of nebula and optical magnitude.) Through our collaborator J.S. Kim (U. AZ.) we have access to CG4 optical data in BVRI filters from the CTIO 0.9m.Extrapolating from this info may permit us to predict where and why new stars form. |
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| + | Conditional on the outcome of the first research step; The second step in our research is to determine whether a Cluster of New Stars exists in the area, and that information may to relevant to the study of Triggered Star Formation.(See “Spitzer Observations of IC 2118.) | ||
Skyview Telescope (http://skyview.gsfc.nasa.gov)) shows radiation at all wavelengths and images at all wavelengths of excited gas/dust in the selected region. In addition, O & B Stars, as well as supernova remnants of their cousin stars, reside in the nearby Vela Nebula. Through our collaborator J.S.Kim (U. AZ) we have access to X-ray data from XMM, Epic and PN images that cover CG4. Their presence may have aided star formation by providing compression pressure onto nebula, or destroyed knots of collapsing dust, by photo evaporation, thus terminating the young stars before they reach The Main Sequence. (UV data source detecting photo evaporation from Determining the distance from CG4 to those O & B stars (using ) will be important to determine what effect that parameter has on star formation. We plan to use Spitzer MIPS data, available in far IR 24, 70, 160 mm wavelengths to detect warm, collapsing gas clouds/protostars. | Skyview Telescope (http://skyview.gsfc.nasa.gov)) shows radiation at all wavelengths and images at all wavelengths of excited gas/dust in the selected region. In addition, O & B Stars, as well as supernova remnants of their cousin stars, reside in the nearby Vela Nebula. Through our collaborator J.S.Kim (U. AZ) we have access to X-ray data from XMM, Epic and PN images that cover CG4. Their presence may have aided star formation by providing compression pressure onto nebula, or destroyed knots of collapsing dust, by photo evaporation, thus terminating the young stars before they reach The Main Sequence. (UV data source detecting photo evaporation from Determining the distance from CG4 to those O & B stars (using ) will be important to determine what effect that parameter has on star formation. We plan to use Spitzer MIPS data, available in far IR 24, 70, 160 mm wavelengths to detect warm, collapsing gas clouds/protostars. | ||
When candidates have been thus identified, POSS (Palomar Observatory Sky Survey) in 8000 mm will reveal the near IR signature of excess IR coming from a newly formed star. | When candidates have been thus identified, POSS (Palomar Observatory Sky Survey) in 8000 mm will reveal the near IR signature of excess IR coming from a newly formed star. | ||
Revision as of 05:48, 8 February 2010
Please see a very raw first cut at writing the Introduction and Background for The Proposal. You already feel free to edit, right? This gives a place to start, or a decision to start over. --Mallory 12:43, 3 February 2010 (PST)
Draft
STAR FORMATION IN CG4
What factors can make Nebulae, ordinary clouds of hydrogen and helium and perhaps some tritium gas, plus dust of common silicate compounds, which appear widely throughout the plane of The Milky Way/or any galaxy, overcome the plentiful disruptive forces in their environment, and form stars? When can the classically interpreted Force of Gravity, overwhelm the dispersive effect of radiation, and force collapse into a star, on a cloud of gas and dust?
And what is the importance of Young Stars, anyway? On the local scale, even small stars usually form discs, which often coalesce into planets. And some may be Earth-Like planets! On a more grand scale, formation and evolution of different types of stars, changes gas and dust and chemical composition of Galaxies; Evolution of the structural components of the universe, i.e. Galaxies, causes evolution of the Universe!
We choose the Cometary Globules CG4 (R. A. 7 degrees 34’ 9”, Dec -56 degrees, Ecliptic Co-ords.) in which to look for new stars. The following is a summary of info describing the CG4- Gum Nebula environment, chosen because the area is visually and photometrically dense with star-forming material. (Used USNO http://www.nofs.navy.mil/data/fchPix to determine opacity of nebula and optical magnitude.) Through our collaborator J.S. Kim (U. AZ.) we have access to CG4 optical data in BVRI filters from the CTIO 0.9m.Extrapolating from this info may permit us to predict where and why new stars form.
Conditional on the outcome of the first research step; The second step in our research is to determine whether a Cluster of New Stars exists in the area, and that information may to relevant to the study of Triggered Star Formation.(See “Spitzer Observations of IC 2118.)
Skyview Telescope (http://skyview.gsfc.nasa.gov)) shows radiation at all wavelengths and images at all wavelengths of excited gas/dust in the selected region. In addition, O & B Stars, as well as supernova remnants of their cousin stars, reside in the nearby Vela Nebula. Through our collaborator J.S.Kim (U. AZ) we have access to X-ray data from XMM, Epic and PN images that cover CG4. Their presence may have aided star formation by providing compression pressure onto nebula, or destroyed knots of collapsing dust, by photo evaporation, thus terminating the young stars before they reach The Main Sequence. (UV data source detecting photo evaporation from Determining the distance from CG4 to those O & B stars (using ) will be important to determine what effect that parameter has on star formation. We plan to use Spitzer MIPS data, available in far IR 24, 70, 160 mm wavelengths to detect warm, collapsing gas clouds/protostars.
When candidates have been thus identified, POSS (Palomar Observatory Sky Survey) in 8000 mm will reveal the near IR signature of excess IR coming from a newly formed star.
