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dc.contributor.authorMoreno-Ibáñez, M.en
dc.contributor.authorGritsevich, M.en
dc.contributor.authorTrigo-Rodríguez, J. M.en
dc.date.accessioned2021-08-31T15:01:59Z-
dc.date.available2021-08-31T15:01:59Z-
dc.date.issued2017-
dc.identifier.citationMoreno-Ibáñez M. Measuring the terminal heights of bolides to understand the atmospheric flight of large asteroidal fragments / M. Moreno-Ibáñez, M. Gritsevich, J. M. Trigo-Rodríguez. — DOI 10.1007/978-3-319-46179-3_7 // Astrophysics and Space Science Proceedings. — 2017. — Vol. 46. — P. 129-151.en
dc.identifier.isbn9783319461786-
dc.identifier.issn15706591-
dc.identifier.otherFinal2
dc.identifier.otherAll Open Access, Green3
dc.identifier.otherhttps://www.scopus.com/inward/record.uri?eid=2-s2.0-85018643081&doi=10.1007%2f978-3-319-46179-3_7&partnerID=40&md5=ffe920e0023605f16515d8d1b439119b
dc.identifier.otherhttps://helda.helsinki.fi/bitstream/10138/310288/1/moreno.pdfm
dc.identifier.urihttp://elar.urfu.ru/handle/10995/102131-
dc.description.abstractThe extent of penetration into the Earth’s atmosphere of a meteoroid is defined by the point where its kinetic energy is no longer sufficient to produce luminosity. For most of the cases this is the point where the meteoroid disintegrates in the atmosphere due to ablation process and dynamic pressure during flight. However, some of these bodies have particular physical properties (bigger size, higher bulk strength, etc.) or favorable flight conditions (lower entry velocity or/and a convenient trajectory slope, etc.) that allow them to become a meteoritedropper and reach the ground. In both cases, we define the end of the luminous path of the trajectory as the terminal height or end height. Thus, the end point shows the amount of deceleration till the final braking. We thus assume that the ability of a fireball to produce meteorites is directly related to its terminal height. Previous studies have discussed the likely relationship between fireball atmospheric flight properties and the terminal height. Most of these studies require the knowledge of a set of properties and physical variables which cannot be determined with sufficient accuracy from ground-based observations. The recently validated dimensionless methodology offers a new approach to this problem. All the unknowns can be reduced to only two parameters which are easily derived from observations. Despite the calculation of the analytic solution of the equations of motion is not trivial, some simplifications are admitted. Here, we describe the best performance range and the errors associated with these simplifications. We discuss how terminal heights depend on two or three variables that are easily retrieved from the recordings, provided at least three trajectory (h, v) points. Additionally, we review the importance of terminal heights, and the way they have been estimated in previous studies. Finally we discuss a new approach for calculating terminal heights. © Springer International Publishing Switzerland 2017.en
dc.format.mimetypeapplication/pdfen
dc.language.isoenen
dc.publisherKluwer Academic Publishersen
dc.rightsinfo:eu-repo/semantics/openAccessen
dc.sourceAstrophysics Space Sci. Proc.2
dc.sourceAstrophysics and Space Science Proceedingsen
dc.subjectASTEROIDSen
dc.subjectEQUATIONS OF MOTIONen
dc.subjectKINETIC ENERGYen
dc.subjectKINETICSen
dc.subjectTRAJECTORIESen
dc.subjectANALYTIC SOLUTIONen
dc.subjectATMOSPHERIC FLIGHTen
dc.subjectDYNAMIC PRESSURESen
dc.subjectENTRY VELOCITYen
dc.subjectFLIGHT CONDITIONSen
dc.subjectGROUND-BASED OBSERVATIONSen
dc.subjectNEW APPROACHESen
dc.subjectPHYSICAL VARIABLESen
dc.subjectEARTH ATMOSPHEREen
dc.titleMeasuring the terminal heights of bolides to understand the atmospheric flight of large asteroidal fragmentsen
dc.typeConference Paperen
dc.typeinfo:eu-repo/semantics/conferenceObjecten
dc.typeinfo:eu-repo/semantics/publishedVersionen
dc.identifier.doi10.1007/978-3-319-46179-3_7-
dc.identifier.scopus85018643081-
local.contributor.employeeMoreno-Ibáñez, M., Institute of Space Sciences (IEEC-CSIC), Meteorites, Minor Bodies and Planetary Sciences Group, Campus UAB, c/Can Magrans s/n, Cerdanyola del Vallés, Barcelona, Catalonia 08193, Spain, Department of Geodesy and Geodynamics, Finnish Geospatial Research Institute (FGI), Geodeetinrinne 2, Masala, FI-02431, Finland
local.contributor.employeeGritsevich, M., Department of Geodesy and Geodynamics, Finnish Geospatial Research Institute (FGI), Geodeetinrinne 2, Masala, FI-02431, Finland, Department of Physics, University of Helsinki, Gustaf Hällströmin katu 2a, P.O. Box 64, Helsinki, FI-00014, Finland, Institute of Physics and Technology, Ural Federal University, Ekaterinburg, 620002, Russian Federation, Department of Computational Physics, Dorodnicyn Computing Centre, Russian Academy of Sciences, Vavilova str. 40, Moscow, 119333, Russian Federation
local.contributor.employeeTrigo-Rodríguez, J.M., Institute of Space Sciences (IEEC-CSIC), Meteorites, Minor Bodies and Planetary Sciences Group, Campus UAB, c/Can Magrans s/n, Cerdanyola del Vallés, Barcelona, Catalonia 08193, Spain
local.description.firstpage129-
local.description.lastpage151-
local.volume46-
local.contributor.departmentInstitute of Space Sciences (IEEC-CSIC), Meteorites, Minor Bodies and Planetary Sciences Group, Campus UAB, c/Can Magrans s/n, Cerdanyola del Vallés, Barcelona, Catalonia 08193, Spain
local.contributor.departmentDepartment of Geodesy and Geodynamics, Finnish Geospatial Research Institute (FGI), Geodeetinrinne 2, Masala, FI-02431, Finland
local.contributor.departmentDepartment of Physics, University of Helsinki, Gustaf Hällströmin katu 2a, P.O. Box 64, Helsinki, FI-00014, Finland
local.contributor.departmentInstitute of Physics and Technology, Ural Federal University, Ekaterinburg, 620002, Russian Federation
local.contributor.departmentDepartment of Computational Physics, Dorodnicyn Computing Centre, Russian Academy of Sciences, Vavilova str. 40, Moscow, 119333, Russian Federation
local.identifier.pure1811242-
local.identifier.pure3a545b4e-0bec-41a2-94bd-3d1c5882a73duuid
local.identifier.eid2-s2.0-85018643081-
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