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Article: Morphology of the red rectangle proto-planetary nebula

TitleMorphology of the red rectangle proto-planetary nebula
Authors
KeywordsPlanetary Nebulae: Individual (Red Rectangle)
Radiative Transfer
Stars: Agb And Post-Agb
Issue Date2011
PublisherInstitute of Physics Publishing, Inc. The Journal's web site is located at http://iopscience.iop.org/0004-637X/
Citation
Astrophysical Journal, 2011, v. 740 n. 1, article no. 27 How to Cite?
AbstractThe morphology of the Red Rectangle (RR) exhibits several singular attributes. Most prominent are a series of linear features perpendicular to the symmetry axis which appear as "ladder rungs" across the nebula. At the edge of each "rung" gas seemingly flows from bright knots in a parabolic shape toward the center of the nebula. We present a new model of the RR which explains these features as a projection effect of the more common concentric arcs seen in other proto-planetary nebulae (e.g., Egg Nebula). Using the three-dimensional morpho-kinematic modeling software SHAPE, we have created a model of the RR that consists of spherical shells evacuated by a bi-conical outflow. When the symmetry axis is oriented perpendicular to the line of sight, the spherical shells become linear, thereby reproducing the "rungs" seen in the RR. When oriented at different inclinations, the linear features become spherical as observed in the Egg Nebula. The model also accurately reproduces the bright knots and the parabolic outflows from these knots that have proven difficult to explain in the past. Using this model, we are able to place a lower limit on the speed of the outflow of 158kms -1. © 2011. The American Astronomical Society. All rights reserved.
Persistent Identifierhttp://hdl.handle.net/10722/179718
ISSN
2015 Impact Factor: 5.909
2015 SCImago Journal Rankings: 3.266
ISI Accession Number ID
Funding AgencyGrant Number
Natural Sciences and Engineering Research Council of Canada (NSERC)
Alberta Ingenuity Fund
Killam Trusts
Research Grants Council of the Hong Kong Special Administrative Region, ChinaHKU 7031/10P
CONACYT49447
UNAMPAPIIT IN100410
Funding Information:

N.K. acknowledges support from the Natural Sciences and Engineering Research Council of Canada (NSERC), the Alberta Ingenuity Fund, and the Killam Trusts. This work was supported by a grant to S.K. from the Research Grants Council of the Hong Kong Special Administrative Region, China (Project No. HKU 7031/10P). W. S. acknowledges support by grants from CONACYT 49447 and UNAM PAPIIT IN100410.

References

 

DC FieldValueLanguage
dc.contributor.authorKoning, Nen_US
dc.contributor.authorKwok, Sen_US
dc.contributor.authorSteffen, Wen_US
dc.date.accessioned2012-12-19T10:03:15Z-
dc.date.available2012-12-19T10:03:15Z-
dc.date.issued2011en_US
dc.identifier.citationAstrophysical Journal, 2011, v. 740 n. 1, article no. 27en_US
dc.identifier.issn0004-637Xen_US
dc.identifier.urihttp://hdl.handle.net/10722/179718-
dc.description.abstractThe morphology of the Red Rectangle (RR) exhibits several singular attributes. Most prominent are a series of linear features perpendicular to the symmetry axis which appear as "ladder rungs" across the nebula. At the edge of each "rung" gas seemingly flows from bright knots in a parabolic shape toward the center of the nebula. We present a new model of the RR which explains these features as a projection effect of the more common concentric arcs seen in other proto-planetary nebulae (e.g., Egg Nebula). Using the three-dimensional morpho-kinematic modeling software SHAPE, we have created a model of the RR that consists of spherical shells evacuated by a bi-conical outflow. When the symmetry axis is oriented perpendicular to the line of sight, the spherical shells become linear, thereby reproducing the "rungs" seen in the RR. When oriented at different inclinations, the linear features become spherical as observed in the Egg Nebula. The model also accurately reproduces the bright knots and the parabolic outflows from these knots that have proven difficult to explain in the past. Using this model, we are able to place a lower limit on the speed of the outflow of 158kms -1. © 2011. The American Astronomical Society. All rights reserved.en_US
dc.languageengen_US
dc.publisherInstitute of Physics Publishing, Inc. The Journal's web site is located at http://iopscience.iop.org/0004-637X/en_US
dc.relation.ispartofAstrophysical Journalen_US
dc.subjectPlanetary Nebulae: Individual (Red Rectangle)en_US
dc.subjectRadiative Transferen_US
dc.subjectStars: Agb And Post-Agben_US
dc.titleMorphology of the red rectangle proto-planetary nebulaen_US
dc.typeArticleen_US
dc.identifier.openurlhttp://library.hku.hk:4550/resserv?sid=HKU:IR&issn=0004-637X&volume=740&issue=1, article no. 27&spage=&epage=&date=2011&atitle=Morphology+of+the+red+rectangle+proto-planetary+nebula-
dc.identifier.emailKwok, S: deannote@hku.hken_US
dc.identifier.authorityKwok, S=rp00716en_US
dc.description.naturelink_to_subscribed_fulltexten_US
dc.identifier.doi10.1088/0004-637X/740/1/27en_US
dc.identifier.scopuseid_2-s2.0-80053469456en_US
dc.identifier.hkuros197164-
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-80053469456&selection=ref&src=s&origin=recordpageen_US
dc.identifier.volume740en_US
dc.identifier.issue1en_US
dc.identifier.isiWOS:000295256500027-
dc.publisher.placeUnited Statesen_US
dc.identifier.scopusauthoridKoning, N=15520613500en_US
dc.identifier.scopusauthoridKwok, S=22980498300en_US
dc.identifier.scopusauthoridSteffen, W=7005295915en_US

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