Loading…
Modeling the Optical to Ultraviolet Polarimetric Variability from Thomson Scattering in Colliding Wind Binaries
Massive star binaries are critical laboratories for measuring masses and stellar wind mass-loss rates. A major challenge is inferring viewing inclination and extracting information about the colliding wind interaction (CWI) region. Polarimetric variability from electron scattering in the highly ioni...
Saved in:
Published in: | arXiv.org 2022-05 |
---|---|
Main Authors: | , , , , , , , |
Format: | Article |
Language: | English |
Subjects: | |
Online Access: | Get full text |
Tags: |
Add Tag
No Tags, Be the first to tag this record!
|
cited_by | |
---|---|
cites | |
container_end_page | |
container_issue | |
container_start_page | |
container_title | arXiv.org |
container_volume | |
creator | Ignace, Richard Fullard, Andrew Shrestha, Manisha Naze, Yael Gayley, Kenneth Hoffman, Jennifer L Lomax, Jamie R St-Louis, Nicole |
description | Massive star binaries are critical laboratories for measuring masses and stellar wind mass-loss rates. A major challenge is inferring viewing inclination and extracting information about the colliding wind interaction (CWI) region. Polarimetric variability from electron scattering in the highly ionized winds provides important diagnostic information about system geometry. We combine for the first time the well-known generalized treatment of \citet{brown_polarisation_1978} for variable polarization from binaries with the semi-analytic solution for the geometry and surface density CWI shock interface between the winds based on Canto et al 1996. Our calculations include some simplifications in the form of inverse square-law wind densities and the assumption of axisymmetry, but in so doing arrive at several robust conclusions. One is that when the winds are nearly equal (e.g., O\,+\,O binaries), the polarization has a relatively mild decline with binary separation. Another is that despite Thomson scattering being a gray opacity, the continuum polarization can show chromatic effects at ultraviolet wavelengths but will be mostly constant at longer wavelengths. Finally, when one wind dominates the other, as for example in WR+OB binaries, the polarization is expected to be larger at wavelengths where the OB component is more luminous, and generally smaller at wavelengths where the WR component is more luminous. This behavior arises because from the perspective of the WR star, the distortion of the scattering envelope from spherical is a minor perturbation situated far from the WR star. By contrast, the polarization contribution from the OB star is dominated by the geometry of the CWI shock. |
doi_str_mv | 10.48550/arxiv.2205.07612 |
format | article |
fullrecord | <record><control><sourceid>proquest</sourceid><recordid>TN_cdi_proquest_journals_2665373716</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><sourcerecordid>2665373716</sourcerecordid><originalsourceid>FETCH-LOGICAL-a526-206114959783c730e815a846e24674ac0f10f59e99b52994f197324441aceb9e3</originalsourceid><addsrcrecordid>eNotjc1KAzEYRYMgWGofwF3A9YzJl7_JUos_hUoFR12WdPqNTUknNZMWfXun6OreuzjnEnLFWSkrpdiNS9_-WAIwVTKjOZyREQjBi0oCXJBJ328ZY6ANKCVGJD7HNQbffdK8QbrYZ9-4QHOkbyEnd_QxYKYvMbjkd5iTb-j7UN3KB59_aJvijtabuOtjR18blzOmk8t3dBpD8OvT-PDdmt75buCwvyTnrQs9Tv5zTOqH-3r6VMwXj7Pp7bxwCnQBTHMurbKmEo0RDCuuXCU1gtRGuoa1nLXKorUrBdbKllsjQErJXYMri2JMrv-0-xS_Dtjn5TYeUjc8LkFrJYwwXItf_LFbAA</addsrcrecordid><sourcetype>Aggregation Database</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype><pqid>2665373716</pqid></control><display><type>article</type><title>Modeling the Optical to Ultraviolet Polarimetric Variability from Thomson Scattering in Colliding Wind Binaries</title><source>Publicly Available Content (ProQuest)</source><creator>Ignace, Richard ; Fullard, Andrew ; Shrestha, Manisha ; Naze, Yael ; Gayley, Kenneth ; Hoffman, Jennifer L ; Lomax, Jamie R ; St-Louis, Nicole</creator><creatorcontrib>Ignace, Richard ; Fullard, Andrew ; Shrestha, Manisha ; Naze, Yael ; Gayley, Kenneth ; Hoffman, Jennifer L ; Lomax, Jamie R ; St-Louis, Nicole</creatorcontrib><description>Massive star binaries are critical laboratories for measuring masses and stellar wind mass-loss rates. A major challenge is inferring viewing inclination and extracting information about the colliding wind interaction (CWI) region. Polarimetric variability from electron scattering in the highly ionized winds provides important diagnostic information about system geometry. We combine for the first time the well-known generalized treatment of \citet{brown_polarisation_1978} for variable polarization from binaries with the semi-analytic solution for the geometry and surface density CWI shock interface between the winds based on Canto et al 1996. Our calculations include some simplifications in the form of inverse square-law wind densities and the assumption of axisymmetry, but in so doing arrive at several robust conclusions. One is that when the winds are nearly equal (e.g., O\,+\,O binaries), the polarization has a relatively mild decline with binary separation. Another is that despite Thomson scattering being a gray opacity, the continuum polarization can show chromatic effects at ultraviolet wavelengths but will be mostly constant at longer wavelengths. Finally, when one wind dominates the other, as for example in WR+OB binaries, the polarization is expected to be larger at wavelengths where the OB component is more luminous, and generally smaller at wavelengths where the WR component is more luminous. This behavior arises because from the perspective of the WR star, the distortion of the scattering envelope from spherical is a minor perturbation situated far from the WR star. By contrast, the polarization contribution from the OB star is dominated by the geometry of the CWI shock.</description><identifier>EISSN: 2331-8422</identifier><identifier>DOI: 10.48550/arxiv.2205.07612</identifier><language>eng</language><publisher>Ithaca: Cornell University Library, arXiv.org</publisher><subject>Binary stars ; Exact solutions ; Geometry ; Massive stars ; Perturbation ; Polarimetry ; Polarization ; Stellar winds ; Thomson scattering ; Variability ; Wavelengths ; Wind</subject><ispartof>arXiv.org, 2022-05</ispartof><rights>2022. This work is published under http://creativecommons.org/licenses/by/4.0/ (the “License”). Notwithstanding the ProQuest Terms and Conditions, you may use this content in accordance with the terms of the License.</rights><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktohtml>$$Uhttps://www.proquest.com/docview/2665373716?pq-origsite=primo$$EHTML$$P50$$Gproquest$$Hfree_for_read</linktohtml><link.rule.ids>780,784,25753,27925,37012,44590</link.rule.ids></links><search><creatorcontrib>Ignace, Richard</creatorcontrib><creatorcontrib>Fullard, Andrew</creatorcontrib><creatorcontrib>Shrestha, Manisha</creatorcontrib><creatorcontrib>Naze, Yael</creatorcontrib><creatorcontrib>Gayley, Kenneth</creatorcontrib><creatorcontrib>Hoffman, Jennifer L</creatorcontrib><creatorcontrib>Lomax, Jamie R</creatorcontrib><creatorcontrib>St-Louis, Nicole</creatorcontrib><title>Modeling the Optical to Ultraviolet Polarimetric Variability from Thomson Scattering in Colliding Wind Binaries</title><title>arXiv.org</title><description>Massive star binaries are critical laboratories for measuring masses and stellar wind mass-loss rates. A major challenge is inferring viewing inclination and extracting information about the colliding wind interaction (CWI) region. Polarimetric variability from electron scattering in the highly ionized winds provides important diagnostic information about system geometry. We combine for the first time the well-known generalized treatment of \citet{brown_polarisation_1978} for variable polarization from binaries with the semi-analytic solution for the geometry and surface density CWI shock interface between the winds based on Canto et al 1996. Our calculations include some simplifications in the form of inverse square-law wind densities and the assumption of axisymmetry, but in so doing arrive at several robust conclusions. One is that when the winds are nearly equal (e.g., O\,+\,O binaries), the polarization has a relatively mild decline with binary separation. Another is that despite Thomson scattering being a gray opacity, the continuum polarization can show chromatic effects at ultraviolet wavelengths but will be mostly constant at longer wavelengths. Finally, when one wind dominates the other, as for example in WR+OB binaries, the polarization is expected to be larger at wavelengths where the OB component is more luminous, and generally smaller at wavelengths where the WR component is more luminous. This behavior arises because from the perspective of the WR star, the distortion of the scattering envelope from spherical is a minor perturbation situated far from the WR star. By contrast, the polarization contribution from the OB star is dominated by the geometry of the CWI shock.</description><subject>Binary stars</subject><subject>Exact solutions</subject><subject>Geometry</subject><subject>Massive stars</subject><subject>Perturbation</subject><subject>Polarimetry</subject><subject>Polarization</subject><subject>Stellar winds</subject><subject>Thomson scattering</subject><subject>Variability</subject><subject>Wavelengths</subject><subject>Wind</subject><issn>2331-8422</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2022</creationdate><recordtype>article</recordtype><sourceid>PIMPY</sourceid><recordid>eNotjc1KAzEYRYMgWGofwF3A9YzJl7_JUos_hUoFR12WdPqNTUknNZMWfXun6OreuzjnEnLFWSkrpdiNS9_-WAIwVTKjOZyREQjBi0oCXJBJ328ZY6ANKCVGJD7HNQbffdK8QbrYZ9-4QHOkbyEnd_QxYKYvMbjkd5iTb-j7UN3KB59_aJvijtabuOtjR18blzOmk8t3dBpD8OvT-PDdmt75buCwvyTnrQs9Tv5zTOqH-3r6VMwXj7Pp7bxwCnQBTHMurbKmEo0RDCuuXCU1gtRGuoa1nLXKorUrBdbKllsjQErJXYMri2JMrv-0-xS_Dtjn5TYeUjc8LkFrJYwwXItf_LFbAA</recordid><startdate>20220516</startdate><enddate>20220516</enddate><creator>Ignace, Richard</creator><creator>Fullard, Andrew</creator><creator>Shrestha, Manisha</creator><creator>Naze, Yael</creator><creator>Gayley, Kenneth</creator><creator>Hoffman, Jennifer L</creator><creator>Lomax, Jamie R</creator><creator>St-Louis, Nicole</creator><general>Cornell University Library, arXiv.org</general><scope>8FE</scope><scope>8FG</scope><scope>ABJCF</scope><scope>ABUWG</scope><scope>AFKRA</scope><scope>AZQEC</scope><scope>BENPR</scope><scope>BGLVJ</scope><scope>CCPQU</scope><scope>DWQXO</scope><scope>HCIFZ</scope><scope>L6V</scope><scope>M7S</scope><scope>PIMPY</scope><scope>PQEST</scope><scope>PQQKQ</scope><scope>PQUKI</scope><scope>PRINS</scope><scope>PTHSS</scope></search><sort><creationdate>20220516</creationdate><title>Modeling the Optical to Ultraviolet Polarimetric Variability from Thomson Scattering in Colliding Wind Binaries</title><author>Ignace, Richard ; Fullard, Andrew ; Shrestha, Manisha ; Naze, Yael ; Gayley, Kenneth ; Hoffman, Jennifer L ; Lomax, Jamie R ; St-Louis, Nicole</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-a526-206114959783c730e815a846e24674ac0f10f59e99b52994f197324441aceb9e3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2022</creationdate><topic>Binary stars</topic><topic>Exact solutions</topic><topic>Geometry</topic><topic>Massive stars</topic><topic>Perturbation</topic><topic>Polarimetry</topic><topic>Polarization</topic><topic>Stellar winds</topic><topic>Thomson scattering</topic><topic>Variability</topic><topic>Wavelengths</topic><topic>Wind</topic><toplevel>online_resources</toplevel><creatorcontrib>Ignace, Richard</creatorcontrib><creatorcontrib>Fullard, Andrew</creatorcontrib><creatorcontrib>Shrestha, Manisha</creatorcontrib><creatorcontrib>Naze, Yael</creatorcontrib><creatorcontrib>Gayley, Kenneth</creatorcontrib><creatorcontrib>Hoffman, Jennifer L</creatorcontrib><creatorcontrib>Lomax, Jamie R</creatorcontrib><creatorcontrib>St-Louis, Nicole</creatorcontrib><collection>ProQuest SciTech Collection</collection><collection>ProQuest Technology Collection</collection><collection>Materials Science & Engineering Collection</collection><collection>ProQuest Central (Alumni)</collection><collection>ProQuest Central</collection><collection>ProQuest Central Essentials</collection><collection>ProQuest Central</collection><collection>Technology Collection</collection><collection>ProQuest One Community College</collection><collection>ProQuest Central</collection><collection>SciTech Premium Collection</collection><collection>ProQuest Engineering Collection</collection><collection>Engineering Database</collection><collection>Publicly Available Content (ProQuest)</collection><collection>ProQuest One Academic Eastern Edition (DO NOT USE)</collection><collection>ProQuest One Academic</collection><collection>ProQuest One Academic UKI Edition</collection><collection>ProQuest Central China</collection><collection>Engineering Collection</collection><jtitle>arXiv.org</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Ignace, Richard</au><au>Fullard, Andrew</au><au>Shrestha, Manisha</au><au>Naze, Yael</au><au>Gayley, Kenneth</au><au>Hoffman, Jennifer L</au><au>Lomax, Jamie R</au><au>St-Louis, Nicole</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Modeling the Optical to Ultraviolet Polarimetric Variability from Thomson Scattering in Colliding Wind Binaries</atitle><jtitle>arXiv.org</jtitle><date>2022-05-16</date><risdate>2022</risdate><eissn>2331-8422</eissn><abstract>Massive star binaries are critical laboratories for measuring masses and stellar wind mass-loss rates. A major challenge is inferring viewing inclination and extracting information about the colliding wind interaction (CWI) region. Polarimetric variability from electron scattering in the highly ionized winds provides important diagnostic information about system geometry. We combine for the first time the well-known generalized treatment of \citet{brown_polarisation_1978} for variable polarization from binaries with the semi-analytic solution for the geometry and surface density CWI shock interface between the winds based on Canto et al 1996. Our calculations include some simplifications in the form of inverse square-law wind densities and the assumption of axisymmetry, but in so doing arrive at several robust conclusions. One is that when the winds are nearly equal (e.g., O\,+\,O binaries), the polarization has a relatively mild decline with binary separation. Another is that despite Thomson scattering being a gray opacity, the continuum polarization can show chromatic effects at ultraviolet wavelengths but will be mostly constant at longer wavelengths. Finally, when one wind dominates the other, as for example in WR+OB binaries, the polarization is expected to be larger at wavelengths where the OB component is more luminous, and generally smaller at wavelengths where the WR component is more luminous. This behavior arises because from the perspective of the WR star, the distortion of the scattering envelope from spherical is a minor perturbation situated far from the WR star. By contrast, the polarization contribution from the OB star is dominated by the geometry of the CWI shock.</abstract><cop>Ithaca</cop><pub>Cornell University Library, arXiv.org</pub><doi>10.48550/arxiv.2205.07612</doi><oa>free_for_read</oa></addata></record> |
fulltext | fulltext |
identifier | EISSN: 2331-8422 |
ispartof | arXiv.org, 2022-05 |
issn | 2331-8422 |
language | eng |
recordid | cdi_proquest_journals_2665373716 |
source | Publicly Available Content (ProQuest) |
subjects | Binary stars Exact solutions Geometry Massive stars Perturbation Polarimetry Polarization Stellar winds Thomson scattering Variability Wavelengths Wind |
title | Modeling the Optical to Ultraviolet Polarimetric Variability from Thomson Scattering in Colliding Wind Binaries |
url | http://sfxeu10.hosted.exlibrisgroup.com/loughborough?ctx_ver=Z39.88-2004&ctx_enc=info:ofi/enc:UTF-8&ctx_tim=2024-12-24T15%3A31%3A25IST&url_ver=Z39.88-2004&url_ctx_fmt=infofi/fmt:kev:mtx:ctx&rfr_id=info:sid/primo.exlibrisgroup.com:primo3-Article-proquest&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.genre=article&rft.atitle=Modeling%20the%20Optical%20to%20Ultraviolet%20Polarimetric%20Variability%20from%20Thomson%20Scattering%20in%20Colliding%20Wind%20Binaries&rft.jtitle=arXiv.org&rft.au=Ignace,%20Richard&rft.date=2022-05-16&rft.eissn=2331-8422&rft_id=info:doi/10.48550/arxiv.2205.07612&rft_dat=%3Cproquest%3E2665373716%3C/proquest%3E%3Cgrp_id%3Ecdi_FETCH-LOGICAL-a526-206114959783c730e815a846e24674ac0f10f59e99b52994f197324441aceb9e3%3C/grp_id%3E%3Coa%3E%3C/oa%3E%3Curl%3E%3C/url%3E&rft_id=info:oai/&rft_pqid=2665373716&rft_id=info:pmid/&rfr_iscdi=true |