Self-Consistent Dynamic Models of Steady Ionization Fronts I. Weak-D and Weak-R Fronts
Astrophys.J. 621 (2005) 328-347 We present a method for including steady-state gas flows in the plasma physics code Cloudy, which was previously restricted to modeling static configurations. The numerical algorithms are described in detail, together with an example application to plane-parallel ioni...
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| creator | Henney, William J Arthur, S. Jane Williams, Robin J. R Ferland, Gary J |
| description | Astrophys.J. 621 (2005) 328-347 We present a method for including steady-state gas flows in the plasma
physics code Cloudy, which was previously restricted to modeling static
configurations. The numerical algorithms are described in detail, together with
an example application to plane-parallel ionization-bounded HII regions. As
well as providing the foundation for future applications to more complex flows,
we find the following specific results regarding the effect of advection upon
ionization fronts in HII regions:
1. Significant direct effects of advection on the global emission properties
occur only when the ionization parameter is lower than is typical for HII
regions.
2. The overheating of partially ionized gas in the front is not large, even
for supersonic (R-type) fronts.
3. The most significant morphological signature of advective fronts is an
electron density spike that occurs at the ionization front. Observational
evidence for such a spike is found in images of the Orion bar.
4. Plane-parallel, weak-D fronts are found to show at best a shallow
correlation between mean velocity and ionization potential for optical emission
lines even when the flow velocity closely approaches the ionized sound speed. |
| doi_str_mv | 10.48550/arxiv.astro-ph/0501034 |
| format | Article |
| fullrecord | <record><control><sourceid>arxiv_GOX</sourceid><recordid>TN_cdi_arxiv_primary_astro_ph_0501034</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><sourcerecordid>astro_ph_0501034</sourcerecordid><originalsourceid>FETCH-arxiv_primary_astro_ph_05010343</originalsourceid><addsrcrecordid>eNqNzrEOgjAUBdAuDkb9Bt_iWCgBEneQyOAiRsfmBUpohD7SNkb8ehPkA5zuTe4dDmP7SATJMU1FiPatXwE6b4mPXShSEYk4WbN7pfqWZ2Scdl4ZD_lkcNA1XKhRvQNqofIKmwlKMvqDXpOBwpLxDsoAHgqfPAc0za9el23LVi32Tu2W3LBDcbplZz475Gj1gHaSs0eOnVw88b-_L4w1RgE</addsrcrecordid><sourcetype>Open Access Repository</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype></control><display><type>article</type><title>Self-Consistent Dynamic Models of Steady Ionization Fronts I. Weak-D and Weak-R Fronts</title><source>arXiv.org</source><creator>Henney, William J ; Arthur, S. Jane ; Williams, Robin J. R ; Ferland, Gary J</creator><creatorcontrib>Henney, William J ; Arthur, S. Jane ; Williams, Robin J. R ; Ferland, Gary J</creatorcontrib><description>Astrophys.J. 621 (2005) 328-347 We present a method for including steady-state gas flows in the plasma
physics code Cloudy, which was previously restricted to modeling static
configurations. The numerical algorithms are described in detail, together with
an example application to plane-parallel ionization-bounded HII regions. As
well as providing the foundation for future applications to more complex flows,
we find the following specific results regarding the effect of advection upon
ionization fronts in HII regions:
1. Significant direct effects of advection on the global emission properties
occur only when the ionization parameter is lower than is typical for HII
regions.
2. The overheating of partially ionized gas in the front is not large, even
for supersonic (R-type) fronts.
3. The most significant morphological signature of advective fronts is an
electron density spike that occurs at the ionization front. Observational
evidence for such a spike is found in images of the Orion bar.
4. Plane-parallel, weak-D fronts are found to show at best a shallow
correlation between mean velocity and ionization potential for optical emission
lines even when the flow velocity closely approaches the ionized sound speed.</description><identifier>DOI: 10.48550/arxiv.astro-ph/0501034</identifier><language>eng</language><subject>Physics - Astrophysics of Galaxies ; Physics - Cosmology and Nongalactic Astrophysics ; Physics - Earth and Planetary Astrophysics ; Physics - High Energy Astrophysical Phenomena ; Physics - Instrumentation and Methods for Astrophysics ; Physics - Solar and Stellar Astrophysics</subject><creationdate>2005-01</creationdate><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>228,230,780,885</link.rule.ids><linktorsrc>$$Uhttps://arxiv.org/abs/astro-ph/0501034$$EView_record_in_Cornell_University$$FView_record_in_$$GCornell_University$$Hfree_for_read</linktorsrc><backlink>$$Uhttps://doi.org/10.1086/427491$$DView published paper (Access to full text may be restricted)$$Hfree_for_read</backlink><backlink>$$Uhttps://doi.org/10.48550/arXiv.astro-ph/0501034$$DView paper in arXiv$$Hfree_for_read</backlink></links><search><creatorcontrib>Henney, William J</creatorcontrib><creatorcontrib>Arthur, S. Jane</creatorcontrib><creatorcontrib>Williams, Robin J. R</creatorcontrib><creatorcontrib>Ferland, Gary J</creatorcontrib><title>Self-Consistent Dynamic Models of Steady Ionization Fronts I. Weak-D and Weak-R Fronts</title><description>Astrophys.J. 621 (2005) 328-347 We present a method for including steady-state gas flows in the plasma
physics code Cloudy, which was previously restricted to modeling static
configurations. The numerical algorithms are described in detail, together with
an example application to plane-parallel ionization-bounded HII regions. As
well as providing the foundation for future applications to more complex flows,
we find the following specific results regarding the effect of advection upon
ionization fronts in HII regions:
1. Significant direct effects of advection on the global emission properties
occur only when the ionization parameter is lower than is typical for HII
regions.
2. The overheating of partially ionized gas in the front is not large, even
for supersonic (R-type) fronts.
3. The most significant morphological signature of advective fronts is an
electron density spike that occurs at the ionization front. Observational
evidence for such a spike is found in images of the Orion bar.
4. Plane-parallel, weak-D fronts are found to show at best a shallow
correlation between mean velocity and ionization potential for optical emission
lines even when the flow velocity closely approaches the ionized sound speed.</description><subject>Physics - Astrophysics of Galaxies</subject><subject>Physics - Cosmology and Nongalactic Astrophysics</subject><subject>Physics - Earth and Planetary Astrophysics</subject><subject>Physics - High Energy Astrophysical Phenomena</subject><subject>Physics - Instrumentation and Methods for Astrophysics</subject><subject>Physics - Solar and Stellar Astrophysics</subject><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2005</creationdate><recordtype>article</recordtype><sourceid>GOX</sourceid><recordid>eNqNzrEOgjAUBdAuDkb9Bt_iWCgBEneQyOAiRsfmBUpohD7SNkb8ehPkA5zuTe4dDmP7SATJMU1FiPatXwE6b4mPXShSEYk4WbN7pfqWZ2Scdl4ZD_lkcNA1XKhRvQNqofIKmwlKMvqDXpOBwpLxDsoAHgqfPAc0za9el23LVi32Tu2W3LBDcbplZz475Gj1gHaSs0eOnVw88b-_L4w1RgE</recordid><startdate>20050104</startdate><enddate>20050104</enddate><creator>Henney, William J</creator><creator>Arthur, S. Jane</creator><creator>Williams, Robin J. R</creator><creator>Ferland, Gary J</creator><scope>GOX</scope></search><sort><creationdate>20050104</creationdate><title>Self-Consistent Dynamic Models of Steady Ionization Fronts I. Weak-D and Weak-R Fronts</title><author>Henney, William J ; Arthur, S. Jane ; Williams, Robin J. R ; Ferland, Gary J</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-arxiv_primary_astro_ph_05010343</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2005</creationdate><topic>Physics - Astrophysics of Galaxies</topic><topic>Physics - Cosmology and Nongalactic Astrophysics</topic><topic>Physics - Earth and Planetary Astrophysics</topic><topic>Physics - High Energy Astrophysical Phenomena</topic><topic>Physics - Instrumentation and Methods for Astrophysics</topic><topic>Physics - Solar and Stellar Astrophysics</topic><toplevel>online_resources</toplevel><creatorcontrib>Henney, William J</creatorcontrib><creatorcontrib>Arthur, S. Jane</creatorcontrib><creatorcontrib>Williams, Robin J. R</creatorcontrib><creatorcontrib>Ferland, Gary J</creatorcontrib><collection>arXiv.org</collection></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext_linktorsrc</fulltext></delivery><addata><au>Henney, William J</au><au>Arthur, S. Jane</au><au>Williams, Robin J. R</au><au>Ferland, Gary J</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Self-Consistent Dynamic Models of Steady Ionization Fronts I. Weak-D and Weak-R Fronts</atitle><date>2005-01-04</date><risdate>2005</risdate><abstract>Astrophys.J. 621 (2005) 328-347 We present a method for including steady-state gas flows in the plasma
physics code Cloudy, which was previously restricted to modeling static
configurations. The numerical algorithms are described in detail, together with
an example application to plane-parallel ionization-bounded HII regions. As
well as providing the foundation for future applications to more complex flows,
we find the following specific results regarding the effect of advection upon
ionization fronts in HII regions:
1. Significant direct effects of advection on the global emission properties
occur only when the ionization parameter is lower than is typical for HII
regions.
2. The overheating of partially ionized gas in the front is not large, even
for supersonic (R-type) fronts.
3. The most significant morphological signature of advective fronts is an
electron density spike that occurs at the ionization front. Observational
evidence for such a spike is found in images of the Orion bar.
4. Plane-parallel, weak-D fronts are found to show at best a shallow
correlation between mean velocity and ionization potential for optical emission
lines even when the flow velocity closely approaches the ionized sound speed.</abstract><doi>10.48550/arxiv.astro-ph/0501034</doi><oa>free_for_read</oa></addata></record> |
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| subjects | Physics - Astrophysics of Galaxies Physics - Cosmology and Nongalactic Astrophysics Physics - Earth and Planetary Astrophysics Physics - High Energy Astrophysical Phenomena Physics - Instrumentation and Methods for Astrophysics Physics - Solar and Stellar Astrophysics |
| title | Self-Consistent Dynamic Models of Steady Ionization Fronts I. Weak-D and Weak-R Fronts |
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