Luminous efficiency based on FRIPON meteors and limitations of ablation models
Context. In meteor physics, the luminous efficiency tau is used to convert the meteor's magnitude to the corresponding meteoroid's mass. However, a lack of sufficiently accurate verification methods or adequate laboratory tests mean that discussions around this parameter are a subject of c...
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| Veröffentlicht in: | Astronomy and astrophysics (Berlin) 2021-06, Vol.650, p.A159, Article 159 |
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| creator | Drolshagen, E. Ott, T. Koschny, D. Drolshagen, G. Vaubaillon, J. Colas, F. Zanda, B. Bouley, S. Jeanne, S. Malgoyre, A. Birlan, M. Vernazza, P. Gardiol, D. Nedelcu, D. A. Rowe, J. Forcier, M. Trigo-Rodriguez, J. M. Pena-Asensio, E. Lamy, H. Ferriere, L. Barghini, D. Carbognani, A. Di Martino, M. Rasetti, S. Valsecchi, G. B. Volpicelli, C. A. Di Carlo, M. Knapic, C. Pratesi, G. Riva, W. Stirpe, G. M. Zorba, S. Hernandez, O. Grandchamps, A. Jehin, E. Jobin, M. King, A. Sanchez-Lavega, A. Toni, A. Rimola, A. Poppe, B. |
| description | Context. In meteor physics, the luminous efficiency tau is used to convert the meteor's magnitude to the corresponding meteoroid's mass. However, a lack of sufficiently accurate verification methods or adequate laboratory tests mean that discussions around this parameter are a subject of controversy. Aims. In this work, we aim to use meteor data obtained by the Fireball Recovery and InterPlanetary Observation to calculate the luminous efficiencies of the recorded meteors. We also show the limitations of the methods presented herein. Methods. Deceleration-based formulas were used to calculate the masses of the pre-atmospheric meteoroids. These can in turn be compared to the meteor brightnesses to assess the luminous efficiencies of the recorded objects. Fragmentation of the meteoroids is not considered within this model. Good measurements of the meteor deceleration are required. Results. We find tau-values, as well as the shape change coefficients, of 294 meteors and fireballs with determined masses in the range of 10 6-100 kg. The derived -values have a median of median = 2:17%. Most of them are of the order of 0.1-10%. We present how our values are obtained, compare them with data reported in the literature, and discuss several methods. A dependence of on the pre-atmospheric velocity of the meteor, ve, is noticeable with a relation of tau = 0:0023 v2:3 e. Furthermore, a dependence of on the initial meteoroid mass, Me, is found with negative linear behaviour in log-log space: tau = 0 :48 M 0:47 e. Conclusions. The higher luminous efficiency of fast meteors could be explained by the higher amount of energy released. Fast meteoroids produce additional emission lines that radiate more efficiently in specific wavelengths due to the appearance of the so-called second component of higher temperature. Furthermore, the negative dependence of on Me implies that the radiation of smaller meteoroids is more efficient. The results of this study also show the limitations of the ablation-based model for the determination of the luminous efficiency. |
| doi_str_mv | 10.1051/0004-6361/202040204 |
| format | Article |
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A. ; Rowe, J. ; Forcier, M. ; Trigo-Rodriguez, J. M. ; Pena-Asensio, E. ; Lamy, H. ; Ferriere, L. ; Barghini, D. ; Carbognani, A. ; Di Martino, M. ; Rasetti, S. ; Valsecchi, G. B. ; Volpicelli, C. A. ; Di Carlo, M. ; Knapic, C. ; Pratesi, G. ; Riva, W. ; Stirpe, G. M. ; Zorba, S. ; Hernandez, O. ; Grandchamps, A. ; Jehin, E. ; Jobin, M. ; King, A. ; Sanchez-Lavega, A. ; Toni, A. ; Rimola, A. ; Poppe, B.</creator><creatorcontrib>Drolshagen, E. ; Ott, T. ; Koschny, D. ; Drolshagen, G. ; Vaubaillon, J. ; Colas, F. ; Zanda, B. ; Bouley, S. ; Jeanne, S. ; Malgoyre, A. ; Birlan, M. ; Vernazza, P. ; Gardiol, D. ; Nedelcu, D. A. ; Rowe, J. ; Forcier, M. ; Trigo-Rodriguez, J. M. ; Pena-Asensio, E. ; Lamy, H. ; Ferriere, L. ; Barghini, D. ; Carbognani, A. ; Di Martino, M. ; Rasetti, S. ; Valsecchi, G. B. ; Volpicelli, C. A. ; Di Carlo, M. ; Knapic, C. ; Pratesi, G. ; Riva, W. ; Stirpe, G. M. ; Zorba, S. ; Hernandez, O. ; Grandchamps, A. ; Jehin, E. ; Jobin, M. ; King, A. ; Sanchez-Lavega, A. ; Toni, A. ; Rimola, A. ; Poppe, B.</creatorcontrib><description>Context. In meteor physics, the luminous efficiency tau is used to convert the meteor's magnitude to the corresponding meteoroid's mass. However, a lack of sufficiently accurate verification methods or adequate laboratory tests mean that discussions around this parameter are a subject of controversy. Aims. In this work, we aim to use meteor data obtained by the Fireball Recovery and InterPlanetary Observation to calculate the luminous efficiencies of the recorded meteors. We also show the limitations of the methods presented herein. Methods. Deceleration-based formulas were used to calculate the masses of the pre-atmospheric meteoroids. These can in turn be compared to the meteor brightnesses to assess the luminous efficiencies of the recorded objects. Fragmentation of the meteoroids is not considered within this model. Good measurements of the meteor deceleration are required. Results. We find tau-values, as well as the shape change coefficients, of 294 meteors and fireballs with determined masses in the range of 10 6-100 kg. The derived -values have a median of median = 2:17%. Most of them are of the order of 0.1-10%. We present how our values are obtained, compare them with data reported in the literature, and discuss several methods. A dependence of on the pre-atmospheric velocity of the meteor, ve, is noticeable with a relation of tau = 0:0023 v2:3 e. Furthermore, a dependence of on the initial meteoroid mass, Me, is found with negative linear behaviour in log-log space: tau = 0 :48 M 0:47 e. Conclusions. The higher luminous efficiency of fast meteors could be explained by the higher amount of energy released. Fast meteoroids produce additional emission lines that radiate more efficiently in specific wavelengths due to the appearance of the so-called second component of higher temperature. Furthermore, the negative dependence of on Me implies that the radiation of smaller meteoroids is more efficient. The results of this study also show the limitations of the ablation-based model for the determination of the luminous efficiency.</description><identifier>ISSN: 0004-6361</identifier><identifier>ISSN: 1432-0746</identifier><identifier>EISSN: 1432-0746</identifier><identifier>EISSN: 1432-0756</identifier><identifier>DOI: 10.1051/0004-6361/202040204</identifier><language>eng</language><publisher>LES ULIS CEDEX A: Edp Sciences S A</publisher><subject><![CDATA[Ablation ; asteroids: general ; Astronomy & Astrophysics ; atmospheric effects ; Atmospheric models ; Aérospatiale, astronomie & astrophysique ; comets: general ; Deceleration ; Efficiency ; Fireballs ; Laboratory tests ; Luminous efficacy ; meteorites ; Meteoroids ; meteors ; Meteors & meteorites ; methods: data analysis ; minor planets ; Physical Sciences ; Physical, chemical, mathematical & earth Sciences ; Physique, chimie, mathématiques & sciences de la terre ; Science & Technology ; Sciences of the Universe ; Space science, astronomy & astrophysics ; techniques: photometric ; Temperature dependence]]></subject><ispartof>Astronomy and astrophysics (Berlin), 2021-06, Vol.650, p.A159, Article 159</ispartof><rights>Copyright EDP Sciences Jun 2021</rights><rights>Distributed under a Creative Commons Attribution 4.0 International License</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>true</woscitedreferencessubscribed><woscitedreferencescount>14</woscitedreferencescount><woscitedreferencesoriginalsourcerecordid>wos000668604100007</woscitedreferencesoriginalsourcerecordid><citedby>FETCH-LOGICAL-c400t-c22fcc9ff773bccfc2e4aef6670e7bf31e7b2a0fddbef7c5b9e1eba177c7dd7c3</citedby><cites>FETCH-LOGICAL-c400t-c22fcc9ff773bccfc2e4aef6670e7bf31e7b2a0fddbef7c5b9e1eba177c7dd7c3</cites><orcidid>0000-0002-7257-2150 ; 0000-0001-5685-7642 ; 0000-0001-6496-0017 ; 0000-0001-5684-9896 ; 0000-0003-1651-0630 ; 0000-0002-3702-8731 ; 0000-0001-8213-3525 ; 0000-0002-7087-5369 ; 0000-0003-1572-0396 ; 0000-0002-2564-6743 ; 0000-0002-4210-7151 ; 0000-0001-8923-488X</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>230,315,781,785,886,3728,27929,27930,39263</link.rule.ids><backlink>$$Uhttps://hal.science/hal-03407196$$DView record in HAL$$Hfree_for_read</backlink></links><search><creatorcontrib>Drolshagen, E.</creatorcontrib><creatorcontrib>Ott, T.</creatorcontrib><creatorcontrib>Koschny, D.</creatorcontrib><creatorcontrib>Drolshagen, G.</creatorcontrib><creatorcontrib>Vaubaillon, J.</creatorcontrib><creatorcontrib>Colas, F.</creatorcontrib><creatorcontrib>Zanda, B.</creatorcontrib><creatorcontrib>Bouley, S.</creatorcontrib><creatorcontrib>Jeanne, S.</creatorcontrib><creatorcontrib>Malgoyre, A.</creatorcontrib><creatorcontrib>Birlan, M.</creatorcontrib><creatorcontrib>Vernazza, P.</creatorcontrib><creatorcontrib>Gardiol, D.</creatorcontrib><creatorcontrib>Nedelcu, D. A.</creatorcontrib><creatorcontrib>Rowe, J.</creatorcontrib><creatorcontrib>Forcier, M.</creatorcontrib><creatorcontrib>Trigo-Rodriguez, J. M.</creatorcontrib><creatorcontrib>Pena-Asensio, E.</creatorcontrib><creatorcontrib>Lamy, H.</creatorcontrib><creatorcontrib>Ferriere, L.</creatorcontrib><creatorcontrib>Barghini, D.</creatorcontrib><creatorcontrib>Carbognani, A.</creatorcontrib><creatorcontrib>Di Martino, M.</creatorcontrib><creatorcontrib>Rasetti, S.</creatorcontrib><creatorcontrib>Valsecchi, G. B.</creatorcontrib><creatorcontrib>Volpicelli, C. A.</creatorcontrib><creatorcontrib>Di Carlo, M.</creatorcontrib><creatorcontrib>Knapic, C.</creatorcontrib><creatorcontrib>Pratesi, G.</creatorcontrib><creatorcontrib>Riva, W.</creatorcontrib><creatorcontrib>Stirpe, G. M.</creatorcontrib><creatorcontrib>Zorba, S.</creatorcontrib><creatorcontrib>Hernandez, O.</creatorcontrib><creatorcontrib>Grandchamps, A.</creatorcontrib><creatorcontrib>Jehin, E.</creatorcontrib><creatorcontrib>Jobin, M.</creatorcontrib><creatorcontrib>King, A.</creatorcontrib><creatorcontrib>Sanchez-Lavega, A.</creatorcontrib><creatorcontrib>Toni, A.</creatorcontrib><creatorcontrib>Rimola, A.</creatorcontrib><creatorcontrib>Poppe, B.</creatorcontrib><title>Luminous efficiency based on FRIPON meteors and limitations of ablation models</title><title>Astronomy and astrophysics (Berlin)</title><addtitle>ASTRON ASTROPHYS</addtitle><description>Context. In meteor physics, the luminous efficiency tau is used to convert the meteor's magnitude to the corresponding meteoroid's mass. However, a lack of sufficiently accurate verification methods or adequate laboratory tests mean that discussions around this parameter are a subject of controversy. Aims. In this work, we aim to use meteor data obtained by the Fireball Recovery and InterPlanetary Observation to calculate the luminous efficiencies of the recorded meteors. We also show the limitations of the methods presented herein. Methods. Deceleration-based formulas were used to calculate the masses of the pre-atmospheric meteoroids. These can in turn be compared to the meteor brightnesses to assess the luminous efficiencies of the recorded objects. Fragmentation of the meteoroids is not considered within this model. Good measurements of the meteor deceleration are required. Results. We find tau-values, as well as the shape change coefficients, of 294 meteors and fireballs with determined masses in the range of 10 6-100 kg. The derived -values have a median of median = 2:17%. Most of them are of the order of 0.1-10%. We present how our values are obtained, compare them with data reported in the literature, and discuss several methods. A dependence of on the pre-atmospheric velocity of the meteor, ve, is noticeable with a relation of tau = 0:0023 v2:3 e. Furthermore, a dependence of on the initial meteoroid mass, Me, is found with negative linear behaviour in log-log space: tau = 0 :48 M 0:47 e. Conclusions. The higher luminous efficiency of fast meteors could be explained by the higher amount of energy released. Fast meteoroids produce additional emission lines that radiate more efficiently in specific wavelengths due to the appearance of the so-called second component of higher temperature. Furthermore, the negative dependence of on Me implies that the radiation of smaller meteoroids is more efficient. The results of this study also show the limitations of the ablation-based model for the determination of the luminous efficiency.</description><subject>Ablation</subject><subject>asteroids: general</subject><subject>Astronomy & Astrophysics</subject><subject>atmospheric effects</subject><subject>Atmospheric models</subject><subject>Aérospatiale, astronomie & astrophysique</subject><subject>comets: general</subject><subject>Deceleration</subject><subject>Efficiency</subject><subject>Fireballs</subject><subject>Laboratory tests</subject><subject>Luminous efficacy</subject><subject>meteorites</subject><subject>Meteoroids</subject><subject>meteors</subject><subject>Meteors & meteorites</subject><subject>methods: data analysis</subject><subject>minor planets</subject><subject>Physical Sciences</subject><subject>Physical, chemical, mathematical & earth Sciences</subject><subject>Physique, chimie, mathématiques & sciences de la terre</subject><subject>Science & Technology</subject><subject>Sciences of the Universe</subject><subject>Space science, astronomy & astrophysics</subject><subject>techniques: photometric</subject><subject>Temperature dependence</subject><issn>0004-6361</issn><issn>1432-0746</issn><issn>1432-0746</issn><issn>1432-0756</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2021</creationdate><recordtype>article</recordtype><sourceid>HGBXW</sourceid><recordid>eNqNkU1P3DAQhi1EJRbaX9CLpZ4QShl_xN4c0QoK0gqqCs6W7YypURJDnID49yQbtL32YHvGep_RzDuEfGfwk0HJzgFAFkoods6Bg5zPAVkxKXgBWqpDstorjshxzk9TytlarMjtdmxjl8ZMMYToI3b-nTqbsaapo1d_bn7f3dIWB0x9praraRPbONghpi7TFKh1zS6hbaqxyV_Jl2CbjN8-3xPycHV5v7kutne_bjYX28JLgKHwnAfvqxC0Fs774DlKi0EpDahdEGy6uYVQ1w6D9qWrkKGzTGuv61p7cULEUreJ-Igm9S6aV26SjUs8No_GeuPQcK7WhismSz1Rpwv11zbmuY-t7d93zPXF1sx_ICRoVqlXNml_LNrnPr2MmAfzlMa-m4YyvCw1yEpW1b8-fJ9y7jHsyzIw82rMbLyZjTf71UzU2UK9oUsh71zHPTkRSq0VSDZFMHe9_n_15nM5mzR2g_gA3wyhlw</recordid><startdate>20210601</startdate><enddate>20210601</enddate><creator>Drolshagen, E.</creator><creator>Ott, T.</creator><creator>Koschny, D.</creator><creator>Drolshagen, G.</creator><creator>Vaubaillon, J.</creator><creator>Colas, F.</creator><creator>Zanda, B.</creator><creator>Bouley, S.</creator><creator>Jeanne, S.</creator><creator>Malgoyre, A.</creator><creator>Birlan, M.</creator><creator>Vernazza, P.</creator><creator>Gardiol, D.</creator><creator>Nedelcu, D. 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A. ; Rowe, J. ; Forcier, M. ; Trigo-Rodriguez, J. M. ; Pena-Asensio, E. ; Lamy, H. ; Ferriere, L. ; Barghini, D. ; Carbognani, A. ; Di Martino, M. ; Rasetti, S. ; Valsecchi, G. B. ; Volpicelli, C. A. ; Di Carlo, M. ; Knapic, C. ; Pratesi, G. ; Riva, W. ; Stirpe, G. M. ; Zorba, S. ; Hernandez, O. ; Grandchamps, A. ; Jehin, E. ; Jobin, M. ; King, A. ; Sanchez-Lavega, A. ; Toni, A. ; Rimola, A. ; Poppe, B.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c400t-c22fcc9ff773bccfc2e4aef6670e7bf31e7b2a0fddbef7c5b9e1eba177c7dd7c3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2021</creationdate><topic>Ablation</topic><topic>asteroids: general</topic><topic>Astronomy & Astrophysics</topic><topic>atmospheric effects</topic><topic>Atmospheric models</topic><topic>Aérospatiale, astronomie & astrophysique</topic><topic>comets: general</topic><topic>Deceleration</topic><topic>Efficiency</topic><topic>Fireballs</topic><topic>Laboratory tests</topic><topic>Luminous efficacy</topic><topic>meteorites</topic><topic>Meteoroids</topic><topic>meteors</topic><topic>Meteors & meteorites</topic><topic>methods: data analysis</topic><topic>minor planets</topic><topic>Physical Sciences</topic><topic>Physical, chemical, mathematical & earth Sciences</topic><topic>Physique, chimie, mathématiques & sciences de la terre</topic><topic>Science & Technology</topic><topic>Sciences of the Universe</topic><topic>Space science, astronomy & astrophysics</topic><topic>techniques: photometric</topic><topic>Temperature dependence</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Drolshagen, E.</creatorcontrib><creatorcontrib>Ott, T.</creatorcontrib><creatorcontrib>Koschny, D.</creatorcontrib><creatorcontrib>Drolshagen, G.</creatorcontrib><creatorcontrib>Vaubaillon, J.</creatorcontrib><creatorcontrib>Colas, F.</creatorcontrib><creatorcontrib>Zanda, B.</creatorcontrib><creatorcontrib>Bouley, S.</creatorcontrib><creatorcontrib>Jeanne, S.</creatorcontrib><creatorcontrib>Malgoyre, A.</creatorcontrib><creatorcontrib>Birlan, M.</creatorcontrib><creatorcontrib>Vernazza, P.</creatorcontrib><creatorcontrib>Gardiol, D.</creatorcontrib><creatorcontrib>Nedelcu, D. 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M.</creatorcontrib><creatorcontrib>Zorba, S.</creatorcontrib><creatorcontrib>Hernandez, O.</creatorcontrib><creatorcontrib>Grandchamps, A.</creatorcontrib><creatorcontrib>Jehin, E.</creatorcontrib><creatorcontrib>Jobin, M.</creatorcontrib><creatorcontrib>King, A.</creatorcontrib><creatorcontrib>Sanchez-Lavega, A.</creatorcontrib><creatorcontrib>Toni, A.</creatorcontrib><creatorcontrib>Rimola, A.</creatorcontrib><creatorcontrib>Poppe, B.</creatorcontrib><collection>Web of Science Core Collection</collection><collection>Science Citation Index Expanded</collection><collection>Web of Science - Science Citation Index Expanded - 2021</collection><collection>CrossRef</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>Hyper Article en Ligne (HAL)</collection><collection>Hyper Article en Ligne (HAL) (Open Access)</collection><collection>Université de Liège - Open Repository and Bibliography (ORBI)</collection><jtitle>Astronomy and astrophysics (Berlin)</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Drolshagen, E.</au><au>Ott, T.</au><au>Koschny, D.</au><au>Drolshagen, G.</au><au>Vaubaillon, J.</au><au>Colas, F.</au><au>Zanda, B.</au><au>Bouley, S.</au><au>Jeanne, S.</au><au>Malgoyre, A.</au><au>Birlan, M.</au><au>Vernazza, P.</au><au>Gardiol, D.</au><au>Nedelcu, D. A.</au><au>Rowe, J.</au><au>Forcier, M.</au><au>Trigo-Rodriguez, J. M.</au><au>Pena-Asensio, E.</au><au>Lamy, H.</au><au>Ferriere, L.</au><au>Barghini, D.</au><au>Carbognani, A.</au><au>Di Martino, M.</au><au>Rasetti, S.</au><au>Valsecchi, G. B.</au><au>Volpicelli, C. A.</au><au>Di Carlo, M.</au><au>Knapic, C.</au><au>Pratesi, G.</au><au>Riva, W.</au><au>Stirpe, G. M.</au><au>Zorba, S.</au><au>Hernandez, O.</au><au>Grandchamps, A.</au><au>Jehin, E.</au><au>Jobin, M.</au><au>King, A.</au><au>Sanchez-Lavega, A.</au><au>Toni, A.</au><au>Rimola, A.</au><au>Poppe, B.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Luminous efficiency based on FRIPON meteors and limitations of ablation models</atitle><jtitle>Astronomy and astrophysics (Berlin)</jtitle><stitle>ASTRON ASTROPHYS</stitle><date>2021-06-01</date><risdate>2021</risdate><volume>650</volume><spage>A159</spage><pages>A159-</pages><artnum>159</artnum><issn>0004-6361</issn><issn>1432-0746</issn><eissn>1432-0746</eissn><eissn>1432-0756</eissn><abstract>Context. In meteor physics, the luminous efficiency tau is used to convert the meteor's magnitude to the corresponding meteoroid's mass. However, a lack of sufficiently accurate verification methods or adequate laboratory tests mean that discussions around this parameter are a subject of controversy. Aims. In this work, we aim to use meteor data obtained by the Fireball Recovery and InterPlanetary Observation to calculate the luminous efficiencies of the recorded meteors. We also show the limitations of the methods presented herein. Methods. Deceleration-based formulas were used to calculate the masses of the pre-atmospheric meteoroids. These can in turn be compared to the meteor brightnesses to assess the luminous efficiencies of the recorded objects. Fragmentation of the meteoroids is not considered within this model. Good measurements of the meteor deceleration are required. Results. We find tau-values, as well as the shape change coefficients, of 294 meteors and fireballs with determined masses in the range of 10 6-100 kg. The derived -values have a median of median = 2:17%. Most of them are of the order of 0.1-10%. We present how our values are obtained, compare them with data reported in the literature, and discuss several methods. A dependence of on the pre-atmospheric velocity of the meteor, ve, is noticeable with a relation of tau = 0:0023 v2:3 e. Furthermore, a dependence of on the initial meteoroid mass, Me, is found with negative linear behaviour in log-log space: tau = 0 :48 M 0:47 e. Conclusions. The higher luminous efficiency of fast meteors could be explained by the higher amount of energy released. Fast meteoroids produce additional emission lines that radiate more efficiently in specific wavelengths due to the appearance of the so-called second component of higher temperature. Furthermore, the negative dependence of on Me implies that the radiation of smaller meteoroids is more efficient. The results of this study also show the limitations of the ablation-based model for the determination of the luminous efficiency.</abstract><cop>LES ULIS CEDEX A</cop><pub>Edp Sciences S A</pub><doi>10.1051/0004-6361/202040204</doi><tpages>17</tpages><orcidid>https://orcid.org/0000-0002-7257-2150</orcidid><orcidid>https://orcid.org/0000-0001-5685-7642</orcidid><orcidid>https://orcid.org/0000-0001-6496-0017</orcidid><orcidid>https://orcid.org/0000-0001-5684-9896</orcidid><orcidid>https://orcid.org/0000-0003-1651-0630</orcidid><orcidid>https://orcid.org/0000-0002-3702-8731</orcidid><orcidid>https://orcid.org/0000-0001-8213-3525</orcidid><orcidid>https://orcid.org/0000-0002-7087-5369</orcidid><orcidid>https://orcid.org/0000-0003-1572-0396</orcidid><orcidid>https://orcid.org/0000-0002-2564-6743</orcidid><orcidid>https://orcid.org/0000-0002-4210-7151</orcidid><orcidid>https://orcid.org/0000-0001-8923-488X</orcidid><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext |
| identifier | ISSN: 0004-6361 |
| ispartof | Astronomy and astrophysics (Berlin), 2021-06, Vol.650, p.A159, Article 159 |
| issn | 0004-6361 1432-0746 1432-0746 1432-0756 |
| language | eng |
| recordid | cdi_webofscience_primary_000668604100007CitationCount |
| source | Bacon EDP Sciences France Licence nationale-ISTEX-PS-Journals-PFISTEX; Elektronische Zeitschriftenbibliothek - Frei zugängliche E-Journals; EDP Sciences; Web of Science - Science Citation Index Expanded - 2021<img src="https://exlibris-pub.s3.amazonaws.com/fromwos-v2.jpg" /> |
| subjects | Ablation asteroids: general Astronomy & Astrophysics atmospheric effects Atmospheric models Aérospatiale, astronomie & astrophysique comets: general Deceleration Efficiency Fireballs Laboratory tests Luminous efficacy meteorites Meteoroids meteors Meteors & meteorites methods: data analysis minor planets Physical Sciences Physical, chemical, mathematical & earth Sciences Physique, chimie, mathématiques & sciences de la terre Science & Technology Sciences of the Universe Space science, astronomy & astrophysics techniques: photometric Temperature dependence |
| title | Luminous efficiency based on FRIPON meteors and limitations of ablation models |
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