Disk Radii and Grain Sizes in Herschel-resolved Debris Disks

<!DOCTYPE html>     <html class="no-js" lang="en">  <head> <title>Disk Radii and Grain Sizes in Herschel-resolved Debris Disks - NASA/ADS</title>  <link rel="apple-touch-icon" sizes="180x180" href="//styles/favicon/apple-touch-icon.png" /> <link rel="icon" type="image/png" sizes="32x32" href="//styles/favicon/favicon-32x32.png" /> <link rel="icon" type="image/png" sizes="16x16" href="//styles/favicon/favicon-16x16.png" /> <link rel="manifest" href="//styles/favicon/site.webmanifest" /> <link rel="mask-icon" href="//styles/favicon/safari-pinned-tab.svg" color="#5bbad5" /> <meta name="apple-mobile-web-app-title" content="NASA ADS" /> <meta name="application-name" content="NASA ADS" /> <meta name="msapplication-TileColor" content="#ffc40d" /> <meta name="theme-color" content="#ffffff" />  <link rel="stylesheet" href="/styles/css/styles.css"> <meta name="robots" content="noarchive"> <link rel="canonical" href="http://ui.adsabs.harvard.edu/abs/2014ApJ...792...65P/abstract"/> <meta name="description" content="The radii of debris disks and the sizes of their dust grains are important tracers of the planetesimal formation mechanisms and physical processes operating in these systems. Here we use a representative sample of 34 debris disks resolved in various Herschel Space Observatory (Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA) programs to constrain the disk radii and the size distribution of their dust. While we modeled disks with both warm and cold components, and identified warm inner disks around about two-thirds of the stars, we focus our analysis only on the cold outer disks, i.e., Kuiper-belt analogs. We derive the disk radii from the resolved images and find a large dispersion for host stars of any spectral class, but no significant trend with the stellar luminosity. This argues against ice lines as a dominant player in setting the debris disk sizes, since the ice line location varies with the luminosity of the central star. Fixing the disk radii to those inferred from the resolved images, we model the spectral energy distribution to determine the dust temperature and the grain size distribution for each target. While the dust temperature systematically increases toward earlier spectral types, the ratio of the dust temperature to the blackbody temperature at the disk radius decreases with the stellar luminosity. This is explained by a clear trend of typical sizes increasing toward more luminous stars. The typical grain sizes are compared to the radiation pressure blowout limit s <SUB>blow</SUB> that is proportional to the stellar luminosity-to-mass ratio and thus also increases toward earlier spectral classes. The grain sizes in the disks of G- to A-stars are inferred to be several times s <SUB>blow</SUB> at all stellar luminosities, in agreement with collisional models of debris disks. The sizes, measured in the units of s <SUB>blow</SUB>, appear to decrease with the luminosity, which may be suggestive of the disk's stirring level increasing toward earlier-type stars. The dust opacity index 尾 ranges between zero and two, and the size distribution index q varies between three and five for all the disks in the sample.">  <meta property="og:type" content="article"> <meta property="og:title" content="Disk Radii and Grain Sizes in Herschel-resolved Debris Disks"> <meta property="og:site_name" content="NASA/ADS"> <meta property="og:description" content="The radii of debris disks and the sizes of their dust grains are important tracers of the planetesimal formation mechanisms and physical processes operating in these systems. Here we use a representative sample of 34 debris disks resolved in various Herschel Space Observatory (Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA) programs to constrain the disk radii and the size distribution of their dust. While we modeled disks with both warm and cold components, and identified warm inner disks around about two-thirds of the stars, we focus our analysis only on the cold outer disks, i.e., Kuiper-belt analogs. We derive the disk radii from the resolved images and find a large dispersion for host stars of any spectral class, but no significant trend with the stellar luminosity. This argues against ice lines as a dominant player in setting the debris disk sizes, since the ice line location varies with the luminosity of the central star. Fixing the disk radii to those inferred from the resolved images, we model the spectral energy distribution to determine the dust temperature and the grain size distribution for each target. While the dust temperature systematically increases toward earlier spectral types, the ratio of the dust temperature to the blackbody temperature at the disk radius decreases with the stellar luminosity. This is explained by a clear trend of typical sizes increasing toward more luminous stars. The typical grain sizes are compared to the radiation pressure blowout limit s <SUB>blow</SUB> that is proportional to the stellar luminosity-to-mass ratio and thus also increases toward earlier spectral classes. The grain sizes in the disks of G- to A-stars are inferred to be several times s <SUB>blow</SUB> at all stellar luminosities, in agreement with collisional models of debris disks. The sizes, measured in the units of s <SUB>blow</SUB>, appear to decrease with the luminosity, which may be suggestive of the disk's stirring level increasing toward earlier-type stars. The dust opacity index 尾 ranges between zero and two, and the size distribution index q varies between three and five for all the disks in the sample."> <meta property="og:url" content="https://ui.adsabs.harvard.edu/abs/2014ApJ...792...65P/abstract"> <meta property="og:image" content="https://ui.adsabs.harvard.edu/styles/img/transparent_logo.svg"> <meta property="article:published_time" content="09/2014"> <meta property="article:author" content="Pawellek, Nicole"> <meta property="article:author" content="Krivov, Alexander V."> <meta property="article:author" content="Marshall, Jonathan P."> <meta property="article:author" content="Montesinos, Benjamin"> <meta property="article:author" content="脕brah谩m, P茅ter"> <meta property="article:author" content="Mo贸r, Attila"> <meta property="article:author" content="Bryden, Geoffrey"> <meta property="article:author" content="Eiroa, Carlos">  <meta name="citation_journal_title" content="The Astrophysical Journal"> <meta name="citation_authors" content="Pawellek, Nicole;Krivov, Alexander V.;Marshall, Jonathan P.;Montesinos, Benjamin;脕brah谩m, P茅ter;Mo贸r, Attila;Bryden, Geoffrey;Eiroa, Carlos"> <meta name="citation_title" content="Disk Radii and Grain Sizes in Herschel-resolved Debris Disks"> <meta name="citation_date" content="09/2014"> <meta name="citation_volume" content="792"> <meta name="citation_issue" content="1"> <meta name="citation_firstpage" content="65"> <meta name="citation_doi" content="10.1088/0004-637X/792/1/65"> <meta name="citation_issn" content="0004-637X"> <meta name="citation_language" content="en"> <meta name="citation_keywords" content="circumstellar matter"> <meta name="citation_keywords" content="infrared: stars"> <meta name="citation_keywords" content="planetary systems"> <meta name="citation_keywords" content="stars: individual: GJ 581 HD 9672 HD 10647 HD 10939 HD 13161 HD 14055 HD 17848 HD 20320 HD 21997 HD 23484 HD 27290 HD 48682 HD 50571 HD 71155 HD 71722 HD 95086 HD 95418 HD 102647 HD 104860 HD 109085 HD 110411 HD 125162 HD 139006 HD 142091 HD 161868 HD 170773 HD 172167 HD 182681 HD 188228 HD 195627 HD 197481 HD 207129 HD 216956 HD 218396"> <meta name="citation_keywords" content="Astrophysics - Solar and Stellar Astrophysics"> <meta name="citation_abstract_html_url" content="https://ui.adsabs.harvard.edu/abs/2014ApJ...792...65P/abstract"> <meta name="citation_publication_date" content="09/2014"> <meta name="citation_pdf_url" content="https://ui.adsabs.harvard.edu/link_gateway/2014ApJ...792...65P/PUB_PDF"> <meta name="citation_arxiv_id" content="arXiv:1407.4579" /> <link title="schema(PRISM)" rel="schema.prism" href="http://prismstandard.org/namespaces/1.2/basic/" /> <meta name="prism.publicationDate" content="09/2014" /> <meta name="prism.publicationName" content="ApJ" /> <meta name="prism.issn" content="0004-637X" /> <meta name="prism.volume" content="792" /> <meta name="prism.startingPage" content="65" /> <link title="schema(DC)" rel="schema.dc" href="http://purl.org/dc/elements/1.1/" /> <meta name="dc.identifier" content="doi:10.1088/0004-637X/792/1/65" /> <meta name="dc.date" content="09/2014" /> <meta name="dc.source" content="ApJ" /> <meta name="dc.title" content="Disk Radii and Grain Sizes in Herschel-resolved Debris Disks" /> <meta name="dc.creator" content="Pawellek, Nicole"> <meta name="dc.creator" content="Krivov, Alexander V."> <meta name="dc.creator" content="Marshall, Jonathan P."> <meta name="dc.creator" content="Montesinos, Benjamin"> <meta name="dc.creator" content="脕brah谩m, P茅ter"> <meta name="dc.creator" content="Mo贸r, Attila"> <meta name="dc.creator" content="Bryden, Geoffrey"> <meta name="dc.creator" content="Eiroa, Carlos">  <meta name="twitter:card" content="summary_large_image"/> <meta name="twitter:description" content="The radii of debris disks and the sizes of their dust grains are important tracers of the planetesimal formation mechanisms and physical processes operating in these systems. Here we use a representative sample of 34 debris disks resolved in various Herschel Space Observatory (Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA) programs to constrain the disk radii and the size distribution of their dust. While we modeled disks with both warm and cold components, and identified warm inner disks around about two-thirds of the stars, we focus our analysis only on the cold outer disks, i.e., Kuiper-belt analogs. We derive the disk radii from the resolved images and find a large dispersion for host stars of any spectral class, but no significant trend with the stellar luminosity. This argues against ice lines as a dominant player in setting the debris disk sizes, since the ice line location varies with the luminosity of the central star. Fixing the disk radii to those inferred from the resolved images, we model the spectral energy distribution to determine the dust temperature and the grain size distribution for each target. While the dust temperature systematically increases toward earlier spectral types, the ratio of the dust temperature to the blackbody temperature at the disk radius decreases with the stellar luminosity. This is explained by a clear trend of typical sizes increasing toward more luminous stars. The typical grain sizes are compared to the radiation pressure blowout limit s <SUB>blow</SUB> that is proportional to the stellar luminosity-to-mass ratio and thus also increases toward earlier spectral classes. The grain sizes in the disks of G- to A-stars are inferred to be several times s <SUB>blow</SUB> at all stellar luminosities, in agreement with collisional models of debris disks. The sizes, measured in the units of s <SUB>blow</SUB>, appear to decrease with the luminosity, which may be suggestive of the disk's stirring level increasing toward earlier-type stars. The dust opacity index 尾 ranges between zero and two, and the size distribution index q varies between three and five for all the disks in the sample."/> <meta name="twitter:title" content="Disk Radii and Grain Sizes in Herschel-resolved Debris Disks"/> <meta name="twitter:site" content="@adsabs"/> <meta name="twitter:domain" content="NASA/ADS"/> <meta name="twitter:image:src" content="https://ui.adsabs.harvard.edu/styles/img/transparent_logo.svg"/> <meta name="twitter:creator" content="@adsabs"/> <meta charset="utf-8"> <meta name="viewport" content="width=device-width, initial-scale=1, shrink-to-fit=no"> <base href="/"> <style> .btn-full-ads { color: #fff !important; background-color: #1a1a1a !important; border-color: #1a1a1a !important; margin-top: 9px !important; padding-bottom: 10px !important; padding-top: 10px !important; } .btn-full-ads:hover, .btn-full-ads:focus, .btn-full-ads:active, .btn-full-ads.active, .open>.dropdown-toggle.btn-full-ads { color: #000 !important; background-color: #ddd !important; 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<li class="author"><a href="/search/?q=author%3A%22Krivov%2C+Alexander+V.%22">Krivov, Alexander V.</a> </li>; <li class="author"><a href="/search/?q=author%3A%22Marshall%2C+Jonathan+P.%22">Marshall, Jonathan P.</a> </li>; <li class="author"><a href="/search/?q=author%3A%22Montesinos%2C+Benjamin%22">Montesinos, Benjamin</a> </li>; <li class="author"><a href="/search/?q=author%3A%22%C3%81brah%C3%A1m%2C+P%C3%A9ter%22">脕brah谩m, P茅ter</a> </li>; <li class="author"><a href="/search/?q=author%3A%22Mo%C3%B3r%2C+Attila%22">Mo贸r, Attila</a> </li>; <li class="author"><a href="/search/?q=author%3A%22Bryden%2C+Geoffrey%22">Bryden, Geoffrey</a> </li>; <li class="author"><a href="/search/?q=author%3A%22Eiroa%2C+Carlos%22">Eiroa, Carlos</a> </li> </ul> </div> <div class="s-abstract-text"> <h4 class="sr-only">Abstract</h4> <p> The radii of debris disks and the sizes of their dust grains are important tracers of the planetesimal formation mechanisms and physical processes operating in these systems. Here we use a representative sample of 34 debris disks resolved in various Herschel Space Observatory (Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA) programs to constrain the disk radii and the size distribution of their dust. While we modeled disks with both warm and cold components, and identified warm inner disks around about two-thirds of the stars, we focus our analysis only on the cold outer disks, i.e., Kuiper-belt analogs. We derive the disk radii from the resolved images and find a large dispersion for host stars of any spectral class, but no significant trend with the stellar luminosity. This argues against ice lines as a dominant player in setting the debris disk sizes, since the ice line location varies with the luminosity of the central star. Fixing the disk radii to those inferred from the resolved images, we model the spectral energy distribution to determine the dust temperature and the grain size distribution for each target. While the dust temperature systematically increases toward earlier spectral types, the ratio of the dust temperature to the blackbody temperature at the disk radius decreases with the stellar luminosity. This is explained by a clear trend of typical sizes increasing toward more luminous stars. The typical grain sizes are compared to the radiation pressure blowout limit s <SUB>blow</SUB> that is proportional to the stellar luminosity-to-mass ratio and thus also increases toward earlier spectral classes. The grain sizes in the disks of G- to A-stars are inferred to be several times s <SUB>blow</SUB> at all stellar luminosities, in agreement with collisional models of debris disks. The sizes, measured in the units of s <SUB>blow</SUB>, appear to decrease with the luminosity, which may be suggestive of the disk's stirring level increasing toward earlier-type stars. The dust opacity index 尾 ranges between zero and two, and the size distribution index q varies between three and five for all the disks in the sample. </p> </div> <br> <dl class="s-abstract-dl-horizontal"> <dt>Publication:</dt> <dd> <div id="article-publication">The Astrophysical Journal</div> </dd> <dt>Pub Date:</dt> <dd>September 2014</dd> <dt>DOI:</dt> <dd> <span> <a href="/link_gateway/2014ApJ...792...65P/doi:10.1088/0004-637X/792/1/65" target="_blank" rel="noopener">10.1088/0004-637X/792/1/65</a> <i class="fa fa-external-link"></i> </span> </dd> <dt>arXiv:</dt> <dd> <span> <a href="/link_gateway/2014ApJ...792...65P/arXiv:1407.4579" target="_blank" rel="noopener">arXiv:1407.4579</a> <i class="fa fa-external-link"></i> </span> </dd> <dt>Bibcode:</dt> <dd> <a href="/abs/2014ApJ...792...65P/abstract"> 2014ApJ...792...65P </a> <i class="icon-help" title="The bibcode is assigned by the ADS as a unique identifier for the paper."></i> </dd> <dt>Keywords:</dt> <dd> <ul class="list-inline"> <li>circumstellar matter;</li> <li>infrared: stars;</li> <li>planetary systems;</li> <li>stars: individual: GJ 581 HD 9672 HD 10647 HD 10939 HD 13161 HD 14055 HD 17848 HD 20320 HD 21997 HD 23484 HD 27290 HD 48682 HD 50571 HD 71155 HD 71722 HD 95086 HD 95418 HD 102647 HD 104860 HD 109085 HD 110411 HD 125162 HD 139006 HD 142091 HD 161868 HD 170773 HD 172167 HD 182681 HD 188228 HD 195627 HD 197481 HD 207129 HD 216956 HD 218396;</li> <li>Astrophysics - Solar and Stellar Astrophysics</li> </ul> </dd> <dt>E-Print:</dt> <dd> accepted for publication in ApJ, 22 pages, 7 figures </dd> </dl> </article> </div> <div data-widget="ShowCitations"></div> <div data-widget="ShowReferences"></div> <div data-widget="ShowCoreads"></div> <div data-widget="ShowSimilar"></div> <div data-widget="ShowTableofcontents"></div> <div data-widget="ShowGraphics"></div> <div data-widget="ShowExportcitation" data-origin="abstract"></div> <div data-widget="ShowMetrics" data-allow-redirect="false"></div> <div 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Disk Radii and Grain Sizes in Herschel-resolved Debris Disks - NASA/ADS