Chromospheric activity among fast-rotating M dwarfs in the open cluster NGC 2516
We report radial velocities (RVs), projected equatorial velocities (v sin i) and Ca ii triplet (CaT) chromospheric activity indices for 237 late-K to mid-M candidate members of the young open cluster NGC 2516. These stars have published rotation periods between 0.1 and 15 d. Intermediate-resolution...
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| Veröffentlicht in: | Monthly notices of the Royal Astronomical Society 2010-09, Vol.407 (1), p.465-478 |
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| description | We report radial velocities (RVs), projected equatorial velocities (v sin i) and Ca ii triplet (CaT) chromospheric activity indices for 237 late-K to mid-M candidate members of the young open cluster NGC 2516. These stars have published rotation periods between 0.1 and 15 d. Intermediate-resolution spectra were obtained using the Giraffe spectrograph at the Very Large Telescope. Membership was confirmed on the basis of their RVs for 210 targets. For these stars, we see a marked increase in the fraction of rapidly rotators as we move to cooler spectral types. About 20 per cent of M0–M1 stars have v sin i > 15 km s−1, increasing to 90 per cent of M4 stars. Activity indices derived from the first two lines of the CaT (8498 and 8542 Å) show differing dependencies on the rotation period and mass for stars lying above and below the fully convective boundary. Higher mass stars, of spectral type K3–M2.5, show chromospheric activity which increases with a decreasing Rossby number (the ratio of period to convective turnover time), saturating for Rossby numbers |
| doi_str_mv | 10.1111/j.1365-2966.2010.16917.x |
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J. ; Jeffries, R. D.</creator><creatorcontrib>Jackson, R. J. ; Jeffries, R. D.</creatorcontrib><description>We report radial velocities (RVs), projected equatorial velocities (v sin i) and Ca ii triplet (CaT) chromospheric activity indices for 237 late-K to mid-M candidate members of the young open cluster NGC 2516. These stars have published rotation periods between 0.1 and 15 d. Intermediate-resolution spectra were obtained using the Giraffe spectrograph at the Very Large Telescope. Membership was confirmed on the basis of their RVs for 210 targets. For these stars, we see a marked increase in the fraction of rapidly rotators as we move to cooler spectral types. About 20 per cent of M0–M1 stars have v sin i > 15 km s−1, increasing to 90 per cent of M4 stars. Activity indices derived from the first two lines of the CaT (8498 and 8542 Å) show differing dependencies on the rotation period and mass for stars lying above and below the fully convective boundary. Higher mass stars, of spectral type K3–M2.5, show chromospheric activity which increases with a decreasing Rossby number (the ratio of period to convective turnover time), saturating for Rossby numbers <0.1. For cooler stars, which are probably fully convective and almost all of which have Rossby numbers <0.1, there is a clear decrease in chromospheric activity as (V−I)0 increases, amounting to a fall of about a factor of 2–3 between spectral types M2.5 and M4. This decrease in activity levels at low Rossby numbers is not seen in X-ray observations of the coronae of cluster M dwarfs or of active field M dwarfs. There is no evidence for supersaturation of chromospheric activity for stars of any spectral type at Rossby numbers <0.01. We suggest that the fall in the limiting level of chromospheric emission beyond spectral type M3 in NGC 2516 is, like the simultaneous increase in rotation rates in field stars, associated with a change in the global magnetic topology as stars approach the fully convective boundary and not due to any decrease in dynamo-generated magnetic flux.</description><identifier>ISSN: 0035-8711</identifier><identifier>EISSN: 1365-2966</identifier><identifier>DOI: 10.1111/j.1365-2966.2010.16917.x</identifier><identifier>CODEN: MNRAA4</identifier><language>eng</language><publisher>Oxford, UK: Blackwell Publishing Ltd</publisher><subject>Astronomy ; Astrophysics ; Earth, ocean, space ; Exact sciences and technology ; Fluid mechanics ; Magnetic fields ; open clusters and associations: individual: NGC 2516 ; Stars & galaxies ; stars: low-mass ; stars: magnetic activity ; stars: rotation</subject><ispartof>Monthly notices of the Royal Astronomical Society, 2010-09, Vol.407 (1), p.465-478</ispartof><rights>2010 The Authors. Journal compilation © 2010 RAS 2010</rights><rights>2010 The Authors. Journal compilation © 2010 RAS</rights><rights>2015 INIST-CNRS</rights><rights>Journal compilation © 2010 RAS</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c4867-a71135b62621fc7d3f4bb40f0c514b0165d47861086bfd480365769d6853855b3</citedby></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://onlinelibrary.wiley.com/doi/pdf/10.1111%2Fj.1365-2966.2010.16917.x$$EPDF$$P50$$Gwiley$$H</linktopdf><linktohtml>$$Uhttps://onlinelibrary.wiley.com/doi/full/10.1111%2Fj.1365-2966.2010.16917.x$$EHTML$$P50$$Gwiley$$H</linktohtml><link.rule.ids>314,780,784,1417,27924,27925,45574,45575</link.rule.ids><backlink>$$Uhttp://pascal-francis.inist.fr/vibad/index.php?action=getRecordDetail&idt=23150889$$DView record in Pascal Francis$$Hfree_for_read</backlink></links><search><creatorcontrib>Jackson, R. J.</creatorcontrib><creatorcontrib>Jeffries, R. D.</creatorcontrib><title>Chromospheric activity among fast-rotating M dwarfs in the open cluster NGC 2516</title><title>Monthly notices of the Royal Astronomical Society</title><addtitle>Monthly Notices of the Royal Astronomical Society</addtitle><addtitle>Monthly Notices of the Royal Astronomical Society</addtitle><description>We report radial velocities (RVs), projected equatorial velocities (v sin i) and Ca ii triplet (CaT) chromospheric activity indices for 237 late-K to mid-M candidate members of the young open cluster NGC 2516. These stars have published rotation periods between 0.1 and 15 d. Intermediate-resolution spectra were obtained using the Giraffe spectrograph at the Very Large Telescope. Membership was confirmed on the basis of their RVs for 210 targets. For these stars, we see a marked increase in the fraction of rapidly rotators as we move to cooler spectral types. About 20 per cent of M0–M1 stars have v sin i > 15 km s−1, increasing to 90 per cent of M4 stars. Activity indices derived from the first two lines of the CaT (8498 and 8542 Å) show differing dependencies on the rotation period and mass for stars lying above and below the fully convective boundary. Higher mass stars, of spectral type K3–M2.5, show chromospheric activity which increases with a decreasing Rossby number (the ratio of period to convective turnover time), saturating for Rossby numbers <0.1. For cooler stars, which are probably fully convective and almost all of which have Rossby numbers <0.1, there is a clear decrease in chromospheric activity as (V−I)0 increases, amounting to a fall of about a factor of 2–3 between spectral types M2.5 and M4. This decrease in activity levels at low Rossby numbers is not seen in X-ray observations of the coronae of cluster M dwarfs or of active field M dwarfs. There is no evidence for supersaturation of chromospheric activity for stars of any spectral type at Rossby numbers <0.01. We suggest that the fall in the limiting level of chromospheric emission beyond spectral type M3 in NGC 2516 is, like the simultaneous increase in rotation rates in field stars, associated with a change in the global magnetic topology as stars approach the fully convective boundary and not due to any decrease in dynamo-generated magnetic flux.</description><subject>Astronomy</subject><subject>Astrophysics</subject><subject>Earth, ocean, space</subject><subject>Exact sciences and technology</subject><subject>Fluid mechanics</subject><subject>Magnetic fields</subject><subject>open clusters and associations: individual: NGC 2516</subject><subject>Stars & galaxies</subject><subject>stars: low-mass</subject><subject>stars: magnetic activity</subject><subject>stars: rotation</subject><issn>0035-8711</issn><issn>1365-2966</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2010</creationdate><recordtype>article</recordtype><recordid>eNp1kUtv1DAUhS1EJYaW_2AhIVYZ7Ni-djZIKNAWqdPylBAby0kcxkMmDnbSzvz7Op1qFiC88eN-5-j6XIQwJUua1pvNkjIQWV4ALHMyv0JB5XL3BC2OhadoQQgTmZKUPkPPY9wQQjjLYYE-levgtz4OaxtcjU09uls37rHZ-v4Xbk0cs-BHM7p0W-HmzoQ2YtfjcW2xH2yP626Kow34-qLEuaBwhk5a00X74nE_Rd_PP3wrL7Orm4uP5burrOYKZGZSK0xUkENO21o2rOVVxUlLakF5RSiIhksFlCio2oYrkv4ioWhACaaEqNgpen3wHYL_M9k46q2Lte0601s_RS2B5FQQLhL58i9y46fQp-a05MCo5AVN0KtHyMTadG0wfe2iHoLbmrDXOUteShWJe3vg7lxn98c6JXqeht7oOXQ9h67naeiHaeidXl1_eTgmA3Yw8NPwH3n2jzypsoPKpbB3R50JvzVIJoW-_PFTy_fkq1qVoD-ze3s1mqU</recordid><startdate>201009</startdate><enddate>201009</enddate><creator>Jackson, R. J.</creator><creator>Jeffries, R. D.</creator><general>Blackwell Publishing Ltd</general><general>Wiley-Blackwell</general><general>Oxford University Press</general><scope>BSCLL</scope><scope>IQODW</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope><scope>7TG</scope><scope>KL.</scope></search><sort><creationdate>201009</creationdate><title>Chromospheric activity among fast-rotating M dwarfs in the open cluster NGC 2516</title><author>Jackson, R. J. ; Jeffries, R. D.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c4867-a71135b62621fc7d3f4bb40f0c514b0165d47861086bfd480365769d6853855b3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2010</creationdate><topic>Astronomy</topic><topic>Astrophysics</topic><topic>Earth, ocean, space</topic><topic>Exact sciences and technology</topic><topic>Fluid mechanics</topic><topic>Magnetic fields</topic><topic>open clusters and associations: individual: NGC 2516</topic><topic>Stars & galaxies</topic><topic>stars: low-mass</topic><topic>stars: magnetic activity</topic><topic>stars: rotation</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Jackson, R. J.</creatorcontrib><creatorcontrib>Jeffries, R. D.</creatorcontrib><collection>Istex</collection><collection>Pascal-Francis</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><jtitle>Monthly notices of the Royal Astronomical Society</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Jackson, R. J.</au><au>Jeffries, R. D.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Chromospheric activity among fast-rotating M dwarfs in the open cluster NGC 2516</atitle><jtitle>Monthly notices of the Royal Astronomical Society</jtitle><stitle>Monthly Notices of the Royal Astronomical Society</stitle><addtitle>Monthly Notices of the Royal Astronomical Society</addtitle><date>2010-09</date><risdate>2010</risdate><volume>407</volume><issue>1</issue><spage>465</spage><epage>478</epage><pages>465-478</pages><issn>0035-8711</issn><eissn>1365-2966</eissn><coden>MNRAA4</coden><abstract>We report radial velocities (RVs), projected equatorial velocities (v sin i) and Ca ii triplet (CaT) chromospheric activity indices for 237 late-K to mid-M candidate members of the young open cluster NGC 2516. These stars have published rotation periods between 0.1 and 15 d. Intermediate-resolution spectra were obtained using the Giraffe spectrograph at the Very Large Telescope. Membership was confirmed on the basis of their RVs for 210 targets. For these stars, we see a marked increase in the fraction of rapidly rotators as we move to cooler spectral types. About 20 per cent of M0–M1 stars have v sin i > 15 km s−1, increasing to 90 per cent of M4 stars. Activity indices derived from the first two lines of the CaT (8498 and 8542 Å) show differing dependencies on the rotation period and mass for stars lying above and below the fully convective boundary. Higher mass stars, of spectral type K3–M2.5, show chromospheric activity which increases with a decreasing Rossby number (the ratio of period to convective turnover time), saturating for Rossby numbers <0.1. For cooler stars, which are probably fully convective and almost all of which have Rossby numbers <0.1, there is a clear decrease in chromospheric activity as (V−I)0 increases, amounting to a fall of about a factor of 2–3 between spectral types M2.5 and M4. This decrease in activity levels at low Rossby numbers is not seen in X-ray observations of the coronae of cluster M dwarfs or of active field M dwarfs. There is no evidence for supersaturation of chromospheric activity for stars of any spectral type at Rossby numbers <0.01. We suggest that the fall in the limiting level of chromospheric emission beyond spectral type M3 in NGC 2516 is, like the simultaneous increase in rotation rates in field stars, associated with a change in the global magnetic topology as stars approach the fully convective boundary and not due to any decrease in dynamo-generated magnetic flux.</abstract><cop>Oxford, UK</cop><pub>Blackwell Publishing Ltd</pub><doi>10.1111/j.1365-2966.2010.16917.x</doi><tpages>14</tpages><oa>free_for_read</oa></addata></record> |
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| subjects | Astronomy Astrophysics Earth, ocean, space Exact sciences and technology Fluid mechanics Magnetic fields open clusters and associations: individual: NGC 2516 Stars & galaxies stars: low-mass stars: magnetic activity stars: rotation |
| title | Chromospheric activity among fast-rotating M dwarfs in the open cluster NGC 2516 |
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