AustralieFrV1, PascalFrancis, Curation, bibRecord, 004124

Population synthesis of double neutron stars

Identifieur interne : 004124 ( PascalFrancis/Curation ); précédent : 004123; suivant : 004125

Population synthesis of double neutron stars

Auteurs : S. Oslowski [Australie] ; T. Bulik [Pologne] ; D. Gondek-Rosinska [Pologne, France] ; K. Belczynski [Pologne, États-Unis]

Source :

Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2011.

RBID : Pascal:11-0208604

Descripteurs français

Pascal (Inist)
- Etoile neutron, Modèle, Galaxies, Pulsar, Accrétion, Champ magnétique, Répartition spatiale, Potentiel gravitationnel, Effet sélection, Binaire, Onde gravitationnelle, Rapport masse, Onde radio, Emission onde.

English descriptors

KwdEn :
- Accretion, Binary stars, Galaxies, Gravitational potential, Gravitational waves, Magnetic fields, Mass ratio, Models, Neutron stars, Pulsars, Radiowave radiation, Selection effect, Spatial distribution, Wave emission.

Abstract

Using the STARTRACK binary population synthesis code we model the population of double neutron stars in the Galaxy. We include a detailed treatment of the spin evolution of each pulsar due to processes such as spin-down and spin-up during accretion events as well as magnetic field decay. We also model the spatial distribution of double neutron stars by including their natal kicks and subsequent propagation in the Galactic gravitational potential. This synthetic pulsar population is compared to the observed sample of double neutron stars taking into account the selection effects of detection in the radio band, to determine the most likely evolutionary parameters. With these parameters we determine the properties of the double neutron star binaries detectable in gravitational waves by the high-frequency interferometers LIGO and VIRGO. In particular, we discuss the distributions of chirp masses and mass ratios in samples selected by their radio or gravitational wave emission.

A01	`01`	`1`		`@0 0035-8711`
A02	`01`			`@0 MNRAA4`
A03		`1`		`@0 Mon. Not. R. Astron. Soc.`
A05				`@2 413`
A06				`@2 1`
A08	`01`	`1`	`ENG`	`@1 Population synthesis of double neutron stars`
A11	`01`	`1`		`@1 OSLOWSKI (S.)`
A11	`02`	`1`		`@1 BULIK (T.)`
A11	`03`	`1`		`@1 GONDEK-ROSINSKA (D.)`
A11	`04`	`1`		`@1 BELCZYNSKI (K.)`
A14	`01`			`@1 Swinburne University of Technology, Centre for Astrophysics and Supercomputing. Mail H39, PO Box 218 @2 VIC 3122 @3 AUS @Z 1 aut.`
A14	`02`			`@1 CSIRO Astronomy and Space Sciences, Australia Telescope National Facility, PO Box 76 @2 Epping, NSW 1710 @3 AUS @Z 1 aut.`
A14	`03`			`@1 Astronomical Observatory, University of Warsaw, Aleje Ujazdowskie 4 @2 00-478 Warsaw @3 POL @Z 2 aut. @Z 4 aut.`
A14	`04`			`@1 Nicolaus Copernicus Astronomical Centre, Bartvcka 18 @2 00716 Warszawa @3 POL @Z 2 aut. @Z 3 aut.`
A14	`05`			`@1 Institute of Astronomy, University of Zielona Gòra, Lubuska 2 @2 65-265 Zielona Gòra @3 POL @Z 3 aut.`
A14	`06`			`@1 LUTH, Observatoire de Paris, Universite Paris 7, Place Jules Janssen @2 92195 Meudon @3 FRA @Z 3 aut.`
A14	`07`			`@1 Department of Physics and Astronomy, University of Texas @2 Brownsville, TX 78520 @3 USA @Z 4 aut.`
A20				`@1 461-479`
A21				`@1 2011`
A23	`01`			`@0 ENG`
A43	`01`			`@1 INIST @2 2067 @5 354000192958730340`
A44				`@0 0000 @1 © 2011 INIST-CNRS. All rights reserved.`
A45				`@0 1 p.1/2`
A47	`01`	`1`		`@0 11-0208604`
A60				`@1 P`
A61				`@0 A`
A64	`01`	`1`		`@0 Monthly Notices of the Royal Astronomical Society`
A66	`01`			`@0 USA`
C01	`01`		`ENG`	@0 Using the STARTRACK binary population synthesis code we model the population of double neutron stars in the Galaxy. We include a detailed treatment of the spin evolution of each pulsar due to processes such as spin-down and spin-up during accretion events as well as magnetic field decay. We also model the spatial distribution of double neutron stars by including their natal kicks and subsequent propagation in the Galactic gravitational potential. This synthetic pulsar population is compared to the observed sample of double neutron stars taking into account the selection effects of detection in the radio band, to determine the most likely evolutionary parameters. With these parameters we determine the properties of the double neutron star binaries detectable in gravitational waves by the high-frequency interferometers LIGO and VIRGO. In particular, we discuss the distributions of chirp masses and mass ratios in samples selected by their radio or gravitational wave emission.
C02	`01`	`3`		`@0 001E03`
C03	`01`	`3`	`FRE`	`@0 Etoile neutron @5 26`
C03	`01`	`3`	`ENG`	`@0 Neutron stars @5 26`
C03	`02`	`X`	`FRE`	`@0 Modèle @5 27`
C03	`02`	`X`	`ENG`	`@0 Models @5 27`
C03	`02`	`X`	`SPA`	`@0 Modelo @5 27`
C03	`03`	`3`	`FRE`	`@0 Galaxies @5 28`
C03	`03`	`3`	`ENG`	`@0 Galaxies @5 28`
C03	`04`	`3`	`FRE`	`@0 Pulsar @5 29`
C03	`04`	`3`	`ENG`	`@0 Pulsars @5 29`
C03	`05`	`3`	`FRE`	`@0 Accrétion @5 30`
C03	`05`	`3`	`ENG`	`@0 Accretion @5 30`
C03	`06`	`3`	`FRE`	`@0 Champ magnétique @5 31`
C03	`06`	`3`	`ENG`	`@0 Magnetic fields @5 31`
C03	`07`	`3`	`FRE`	`@0 Répartition spatiale @5 32`
C03	`07`	`3`	`ENG`	`@0 Spatial distribution @5 32`
C03	`08`	`3`	`FRE`	`@0 Potentiel gravitationnel @5 33`
C03	`08`	`3`	`ENG`	`@0 Gravitational potential @5 33`
C03	`09`	`X`	`FRE`	`@0 Effet sélection @5 34`
C03	`09`	`X`	`ENG`	`@0 Selection effect @5 34`
C03	`09`	`X`	`SPA`	`@0 Efecto selección @5 34`
C03	`10`	`3`	`FRE`	`@0 Binaire @5 35`
C03	`10`	`3`	`ENG`	`@0 Binary stars @5 35`
C03	`11`	`3`	`FRE`	`@0 Onde gravitationnelle @5 36`
C03	`11`	`3`	`ENG`	`@0 Gravitational waves @5 36`
C03	`12`	`X`	`FRE`	`@0 Rapport masse @5 37`
C03	`12`	`X`	`ENG`	`@0 Mass ratio @5 37`
C03	`12`	`X`	`SPA`	`@0 Relación masa @5 37`
C03	`13`	`3`	`FRE`	`@0 Onde radio @5 38`
C03	`13`	`3`	`ENG`	`@0 Radiowave radiation @5 38`
C03	`14`	`X`	`FRE`	`@0 Emission onde @5 39`
C03	`14`	`X`	`ENG`	`@0 Wave emission @5 39`
C03	`14`	`X`	`SPA`	`@0 Emisión onda @5 39`
N21				`@1 136`
N44	`01`			`@1 OTO`
N82				`@1 OTO`

Links toward previous steps (curation, corpus...)

to stream PascalFrancis, to step Corpus: Pour aller vers cette notice dans l'étape Curation :001E16

Links to Exploration step

Pascal:11-0208604

Le document en format XML

<record><TEI><teiHeader><fileDesc><titleStmt><title xml:lang="en" level="a">Population synthesis of double neutron stars</title>
<author><name sortKey="Oslowski, S" sort="Oslowski, S" uniqKey="Oslowski S" first="S." last="Oslowski">S. Oslowski</name>
<affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Swinburne University of Technology, Centre for Astrophysics and Supercomputing. Mail H39, PO Box 218</s1>
<s2>VIC 3122</s2>
<s3>AUS</s3>
<sZ>1 aut.</sZ>
</inist:fA14>
<country>Australie</country>
</affiliation>
<affiliation wicri:level="1"><inist:fA14 i1="02"><s1>CSIRO Astronomy and Space Sciences, Australia Telescope National Facility, PO Box 76</s1>
<s2>Epping, NSW 1710</s2>
<s3>AUS</s3>
<sZ>1 aut.</sZ>
</inist:fA14>
<country>Australie</country>
</affiliation>
</author>
<author><name sortKey="Bulik, T" sort="Bulik, T" uniqKey="Bulik T" first="T." last="Bulik">T. Bulik</name>
<affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Astronomical Observatory, University of Warsaw, Aleje Ujazdowskie 4</s1>
<s2>00-478 Warsaw</s2>
<s3>POL</s3>
<sZ>2 aut.</sZ>
<sZ>4 aut.</sZ>
</inist:fA14>
<country>Pologne</country>
</affiliation>
<affiliation wicri:level="1"><inist:fA14 i1="04"><s1>Nicolaus Copernicus Astronomical Centre, Bartvcka 18</s1>
<s2>00716 Warszawa</s2>
<s3>POL</s3>
<sZ>2 aut.</sZ>
<sZ>3 aut.</sZ>
</inist:fA14>
<country>Pologne</country>
</affiliation>
</author>
<author><name sortKey="Gondek Rosinska, D" sort="Gondek Rosinska, D" uniqKey="Gondek Rosinska D" first="D." last="Gondek-Rosinska">D. Gondek-Rosinska</name>
<affiliation wicri:level="1"><inist:fA14 i1="04"><s1>Nicolaus Copernicus Astronomical Centre, Bartvcka 18</s1>
<s2>00716 Warszawa</s2>
<s3>POL</s3>
<sZ>2 aut.</sZ>
<sZ>3 aut.</sZ>
</inist:fA14>
<country>Pologne</country>
</affiliation>
<affiliation wicri:level="1"><inist:fA14 i1="05"><s1>Institute of Astronomy, University of Zielona Gòra, Lubuska 2</s1>
<s2>65-265 Zielona Gòra</s2>
<s3>POL</s3>
<sZ>3 aut.</sZ>
</inist:fA14>
<country>Pologne</country>
</affiliation>
<affiliation wicri:level="1"><inist:fA14 i1="06"><s1>LUTH, Observatoire de Paris, Universite Paris 7, Place Jules Janssen</s1>
<s2>92195 Meudon</s2>
<s3>FRA</s3>
<sZ>3 aut.</sZ>
</inist:fA14>
<country>France</country>
</affiliation>
</author>
<author><name sortKey="Belczynski, K" sort="Belczynski, K" uniqKey="Belczynski K" first="K." last="Belczynski">K. Belczynski</name>
<affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Astronomical Observatory, University of Warsaw, Aleje Ujazdowskie 4</s1>
<s2>00-478 Warsaw</s2>
<s3>POL</s3>
<sZ>2 aut.</sZ>
<sZ>4 aut.</sZ>
</inist:fA14>
<country>Pologne</country>
</affiliation>
<affiliation wicri:level="1"><inist:fA14 i1="07"><s1>Department of Physics and Astronomy, University of Texas</s1>
<s2>Brownsville, TX 78520</s2>
<s3>USA</s3>
<sZ>4 aut.</sZ>
</inist:fA14>
<country>États-Unis</country>
</affiliation>
</author>
</titleStmt>
<publicationStmt><idno type="wicri:source">INIST</idno>
<idno type="inist">11-0208604</idno>
<date when="2011">2011</date>
<idno type="stanalyst">PASCAL 11-0208604 INIST</idno>
<idno type="RBID">Pascal:11-0208604</idno>
<idno type="wicri:Area/PascalFrancis/Corpus">001E16</idno>
<idno type="wicri:Area/PascalFrancis/Curation">004124</idno>
</publicationStmt>
<sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">Population synthesis of double neutron stars</title>
<author><name sortKey="Oslowski, S" sort="Oslowski, S" uniqKey="Oslowski S" first="S." last="Oslowski">S. Oslowski</name>
<affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Swinburne University of Technology, Centre for Astrophysics and Supercomputing. Mail H39, PO Box 218</s1>
<s2>VIC 3122</s2>
<s3>AUS</s3>
<sZ>1 aut.</sZ>
</inist:fA14>
<country>Australie</country>
</affiliation>
<affiliation wicri:level="1"><inist:fA14 i1="02"><s1>CSIRO Astronomy and Space Sciences, Australia Telescope National Facility, PO Box 76</s1>
<s2>Epping, NSW 1710</s2>
<s3>AUS</s3>
<sZ>1 aut.</sZ>
</inist:fA14>
<country>Australie</country>
</affiliation>
</author>
<author><name sortKey="Bulik, T" sort="Bulik, T" uniqKey="Bulik T" first="T." last="Bulik">T. Bulik</name>
<affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Astronomical Observatory, University of Warsaw, Aleje Ujazdowskie 4</s1>
<s2>00-478 Warsaw</s2>
<s3>POL</s3>
<sZ>2 aut.</sZ>
<sZ>4 aut.</sZ>
</inist:fA14>
<country>Pologne</country>
</affiliation>
<affiliation wicri:level="1"><inist:fA14 i1="04"><s1>Nicolaus Copernicus Astronomical Centre, Bartvcka 18</s1>
<s2>00716 Warszawa</s2>
<s3>POL</s3>
<sZ>2 aut.</sZ>
<sZ>3 aut.</sZ>
</inist:fA14>
<country>Pologne</country>
</affiliation>
</author>
<author><name sortKey="Gondek Rosinska, D" sort="Gondek Rosinska, D" uniqKey="Gondek Rosinska D" first="D." last="Gondek-Rosinska">D. Gondek-Rosinska</name>
<affiliation wicri:level="1"><inist:fA14 i1="04"><s1>Nicolaus Copernicus Astronomical Centre, Bartvcka 18</s1>
<s2>00716 Warszawa</s2>
<s3>POL</s3>
<sZ>2 aut.</sZ>
<sZ>3 aut.</sZ>
</inist:fA14>
<country>Pologne</country>
</affiliation>
<affiliation wicri:level="1"><inist:fA14 i1="05"><s1>Institute of Astronomy, University of Zielona Gòra, Lubuska 2</s1>
<s2>65-265 Zielona Gòra</s2>
<s3>POL</s3>
<sZ>3 aut.</sZ>
</inist:fA14>
<country>Pologne</country>
</affiliation>
<affiliation wicri:level="1"><inist:fA14 i1="06"><s1>LUTH, Observatoire de Paris, Universite Paris 7, Place Jules Janssen</s1>
<s2>92195 Meudon</s2>
<s3>FRA</s3>
<sZ>3 aut.</sZ>
</inist:fA14>
<country>France</country>
</affiliation>
</author>
<author><name sortKey="Belczynski, K" sort="Belczynski, K" uniqKey="Belczynski K" first="K." last="Belczynski">K. Belczynski</name>
<affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Astronomical Observatory, University of Warsaw, Aleje Ujazdowskie 4</s1>
<s2>00-478 Warsaw</s2>
<s3>POL</s3>
<sZ>2 aut.</sZ>
<sZ>4 aut.</sZ>
</inist:fA14>
<country>Pologne</country>
</affiliation>
<affiliation wicri:level="1"><inist:fA14 i1="07"><s1>Department of Physics and Astronomy, University of Texas</s1>
<s2>Brownsville, TX 78520</s2>
<s3>USA</s3>
<sZ>4 aut.</sZ>
</inist:fA14>
<country>États-Unis</country>
</affiliation>
</author>
</analytic>
<series><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title>
<title level="j" type="abbreviated">Mon. Not. R. Astron. Soc.</title>
<idno type="ISSN">0035-8711</idno>
<imprint><date when="2011">2011</date>
</imprint>
</series>
</biblStruct>
</sourceDesc>
<seriesStmt><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title>
<title level="j" type="abbreviated">Mon. Not. R. Astron. Soc.</title>
<idno type="ISSN">0035-8711</idno>
</seriesStmt>
</fileDesc>
<profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Accretion</term>
<term>Binary stars</term>
<term>Galaxies</term>
<term>Gravitational potential</term>
<term>Gravitational waves</term>
<term>Magnetic fields</term>
<term>Mass ratio</term>
<term>Models</term>
<term>Neutron stars</term>
<term>Pulsars</term>
<term>Radiowave radiation</term>
<term>Selection effect</term>
<term>Spatial distribution</term>
<term>Wave emission</term>
</keywords>
<keywords scheme="Pascal" xml:lang="fr"><term>Etoile neutron</term>
<term>Modèle</term>
<term>Galaxies</term>
<term>Pulsar</term>
<term>Accrétion</term>
<term>Champ magnétique</term>
<term>Répartition spatiale</term>
<term>Potentiel gravitationnel</term>
<term>Effet sélection</term>
<term>Binaire</term>
<term>Onde gravitationnelle</term>
<term>Rapport masse</term>
<term>Onde radio</term>
<term>Emission onde</term>
</keywords>
</textClass>
</profileDesc>
</teiHeader>
<front><div type="abstract" xml:lang="en">Using the STARTRACK binary population synthesis code we model the population of double neutron stars in the Galaxy. We include a detailed treatment of the spin evolution of each pulsar due to processes such as spin-down and spin-up during accretion events as well as magnetic field decay. We also model the spatial distribution of double neutron stars by including their natal kicks and subsequent propagation in the Galactic gravitational potential. This synthetic pulsar population is compared to the observed sample of double neutron stars taking into account the selection effects of detection in the radio band, to determine the most likely evolutionary parameters. With these parameters we determine the properties of the double neutron star binaries detectable in gravitational waves by the high-frequency interferometers LIGO and VIRGO. In particular, we discuss the distributions of chirp masses and mass ratios in samples selected by their radio or gravitational wave emission.</div>
</front>
</TEI>
<inist><standard h6="B"><pA><fA01 i1="01" i2="1"><s0>0035-8711</s0>
</fA01>
<fA02 i1="01"><s0>MNRAA4</s0>
</fA02>
<fA03 i2="1"><s0>Mon. Not. R. Astron. Soc.</s0>
</fA03>
<fA05><s2>413</s2>
</fA05>
<fA06><s2>1</s2>
</fA06>
<fA08 i1="01" i2="1" l="ENG"><s1>Population synthesis of double neutron stars</s1>
</fA08>
<fA11 i1="01" i2="1"><s1>OSLOWSKI (S.)</s1>
</fA11>
<fA11 i1="02" i2="1"><s1>BULIK (T.)</s1>
</fA11>
<fA11 i1="03" i2="1"><s1>GONDEK-ROSINSKA (D.)</s1>
</fA11>
<fA11 i1="04" i2="1"><s1>BELCZYNSKI (K.)</s1>
</fA11>
<fA14 i1="01"><s1>Swinburne University of Technology, Centre for Astrophysics and Supercomputing. Mail H39, PO Box 218</s1>
<s2>VIC 3122</s2>
<s3>AUS</s3>
<sZ>1 aut.</sZ>
</fA14>
<fA14 i1="02"><s1>CSIRO Astronomy and Space Sciences, Australia Telescope National Facility, PO Box 76</s1>
<s2>Epping, NSW 1710</s2>
<s3>AUS</s3>
<sZ>1 aut.</sZ>
</fA14>
<fA14 i1="03"><s1>Astronomical Observatory, University of Warsaw, Aleje Ujazdowskie 4</s1>
<s2>00-478 Warsaw</s2>
<s3>POL</s3>
<sZ>2 aut.</sZ>
<sZ>4 aut.</sZ>
</fA14>
<fA14 i1="04"><s1>Nicolaus Copernicus Astronomical Centre, Bartvcka 18</s1>
<s2>00716 Warszawa</s2>
<s3>POL</s3>
<sZ>2 aut.</sZ>
<sZ>3 aut.</sZ>
</fA14>
<fA14 i1="05"><s1>Institute of Astronomy, University of Zielona Gòra, Lubuska 2</s1>
<s2>65-265 Zielona Gòra</s2>
<s3>POL</s3>
<sZ>3 aut.</sZ>
</fA14>
<fA14 i1="06"><s1>LUTH, Observatoire de Paris, Universite Paris 7, Place Jules Janssen</s1>
<s2>92195 Meudon</s2>
<s3>FRA</s3>
<sZ>3 aut.</sZ>
</fA14>
<fA14 i1="07"><s1>Department of Physics and Astronomy, University of Texas</s1>
<s2>Brownsville, TX 78520</s2>
<s3>USA</s3>
<sZ>4 aut.</sZ>
</fA14>
<fA20><s1>461-479</s1>
</fA20>
<fA21><s1>2011</s1>
</fA21>
<fA23 i1="01"><s0>ENG</s0>
</fA23>
<fA43 i1="01"><s1>INIST</s1>
<s2>2067</s2>
<s5>354000192958730340</s5>
</fA43>
<fA44><s0>0000</s0>
<s1>© 2011 INIST-CNRS. All rights reserved.</s1>
</fA44>
<fA45><s0>1 p.1/2</s0>
</fA45>
<fA47 i1="01" i2="1"><s0>11-0208604</s0>
</fA47>
<fA60><s1>P</s1>
</fA60>
<fA61><s0>A</s0>
</fA61>
<fA64 i1="01" i2="1"><s0>Monthly Notices of the Royal Astronomical Society</s0>
</fA64>
<fA66 i1="01"><s0>USA</s0>
</fA66>
<fC01 i1="01" l="ENG"><s0>Using the STARTRACK binary population synthesis code we model the population of double neutron stars in the Galaxy. We include a detailed treatment of the spin evolution of each pulsar due to processes such as spin-down and spin-up during accretion events as well as magnetic field decay. We also model the spatial distribution of double neutron stars by including their natal kicks and subsequent propagation in the Galactic gravitational potential. This synthetic pulsar population is compared to the observed sample of double neutron stars taking into account the selection effects of detection in the radio band, to determine the most likely evolutionary parameters. With these parameters we determine the properties of the double neutron star binaries detectable in gravitational waves by the high-frequency interferometers LIGO and VIRGO. In particular, we discuss the distributions of chirp masses and mass ratios in samples selected by their radio or gravitational wave emission.</s0>
</fC01>
<fC02 i1="01" i2="3"><s0>001E03</s0>
</fC02>
<fC03 i1="01" i2="3" l="FRE"><s0>Etoile neutron</s0>
<s5>26</s5>
</fC03>
<fC03 i1="01" i2="3" l="ENG"><s0>Neutron stars</s0>
<s5>26</s5>
</fC03>
<fC03 i1="02" i2="X" l="FRE"><s0>Modèle</s0>
<s5>27</s5>
</fC03>
<fC03 i1="02" i2="X" l="ENG"><s0>Models</s0>
<s5>27</s5>
</fC03>
<fC03 i1="02" i2="X" l="SPA"><s0>Modelo</s0>
<s5>27</s5>
</fC03>
<fC03 i1="03" i2="3" l="FRE"><s0>Galaxies</s0>
<s5>28</s5>
</fC03>
<fC03 i1="03" i2="3" l="ENG"><s0>Galaxies</s0>
<s5>28</s5>
</fC03>
<fC03 i1="04" i2="3" l="FRE"><s0>Pulsar</s0>
<s5>29</s5>
</fC03>
<fC03 i1="04" i2="3" l="ENG"><s0>Pulsars</s0>
<s5>29</s5>
</fC03>
<fC03 i1="05" i2="3" l="FRE"><s0>Accrétion</s0>
<s5>30</s5>
</fC03>
<fC03 i1="05" i2="3" l="ENG"><s0>Accretion</s0>
<s5>30</s5>
</fC03>
<fC03 i1="06" i2="3" l="FRE"><s0>Champ magnétique</s0>
<s5>31</s5>
</fC03>
<fC03 i1="06" i2="3" l="ENG"><s0>Magnetic fields</s0>
<s5>31</s5>
</fC03>
<fC03 i1="07" i2="3" l="FRE"><s0>Répartition spatiale</s0>
<s5>32</s5>
</fC03>
<fC03 i1="07" i2="3" l="ENG"><s0>Spatial distribution</s0>
<s5>32</s5>
</fC03>
<fC03 i1="08" i2="3" l="FRE"><s0>Potentiel gravitationnel</s0>
<s5>33</s5>
</fC03>
<fC03 i1="08" i2="3" l="ENG"><s0>Gravitational potential</s0>
<s5>33</s5>
</fC03>
<fC03 i1="09" i2="X" l="FRE"><s0>Effet sélection</s0>
<s5>34</s5>
</fC03>
<fC03 i1="09" i2="X" l="ENG"><s0>Selection effect</s0>
<s5>34</s5>
</fC03>
<fC03 i1="09" i2="X" l="SPA"><s0>Efecto selección</s0>
<s5>34</s5>
</fC03>
<fC03 i1="10" i2="3" l="FRE"><s0>Binaire</s0>
<s5>35</s5>
</fC03>
<fC03 i1="10" i2="3" l="ENG"><s0>Binary stars</s0>
<s5>35</s5>
</fC03>
<fC03 i1="11" i2="3" l="FRE"><s0>Onde gravitationnelle</s0>
<s5>36</s5>
</fC03>
<fC03 i1="11" i2="3" l="ENG"><s0>Gravitational waves</s0>
<s5>36</s5>
</fC03>
<fC03 i1="12" i2="X" l="FRE"><s0>Rapport masse</s0>
<s5>37</s5>
</fC03>
<fC03 i1="12" i2="X" l="ENG"><s0>Mass ratio</s0>
<s5>37</s5>
</fC03>
<fC03 i1="12" i2="X" l="SPA"><s0>Relación masa</s0>
<s5>37</s5>
</fC03>
<fC03 i1="13" i2="3" l="FRE"><s0>Onde radio</s0>
<s5>38</s5>
</fC03>
<fC03 i1="13" i2="3" l="ENG"><s0>Radiowave radiation</s0>
<s5>38</s5>
</fC03>
<fC03 i1="14" i2="X" l="FRE"><s0>Emission onde</s0>
<s5>39</s5>
</fC03>
<fC03 i1="14" i2="X" l="ENG"><s0>Wave emission</s0>
<s5>39</s5>
</fC03>
<fC03 i1="14" i2="X" l="SPA"><s0>Emisión onda</s0>
<s5>39</s5>
</fC03>
<fN21><s1>136</s1>
</fN21>
<fN44 i1="01"><s1>OTO</s1>
</fN44>
<fN82><s1>OTO</s1>
</fN82>
</pA>
</standard>
</inist>
</record>

Pour manipuler ce document sous Unix (Dilib)

EXPLOR_STEP=$WICRI_ROOT/Wicri/Asie/explor/AustralieFrV1/Data/PascalFrancis/Curation

HfdSelect -h $EXPLOR_STEP/biblio.hfd -nk 004124 | SxmlIndent | more

HfdSelect -h $EXPLOR_AREA/Data/PascalFrancis/Curation/biblio.hfd -nk 004124 | SxmlIndent | more

Pour mettre un lien sur cette page dans le réseau Wicri

{{Explor lien
   |wiki=    Wicri/Asie
   |area=    AustralieFrV1
   |flux=    PascalFrancis
   |étape=   Curation
   |type=    RBID
   |clé=     Pascal:11-0208604
   |texte=   Population synthesis of double neutron stars
}}

This area was generated with Dilib version V0.6.33.
Data generation: Tue Dec 5 10:43:12 2017. Site generation: Tue Mar 5 14:07:20 2024

	Serveur d'exploration sur les relations entre la France et l'Australie
	Attention, ce site est en cours de développement ! Attention, site généré par des moyens informatiques à partir de corpus bruts. Les informations ne sont donc pas validées.

Serveur d'exploration sur les relations entre la France et l'Australie

Population synthesis of double neutron stars

Population synthesis of double neutron stars

Source :

Descripteurs français

English descriptors

Abstract

Links toward previous steps (curation, corpus...)

Links to Exploration step

Le document en format XML

Pour manipuler ce document sous Unix (Dilib)

Pour mettre un lien sur cette page dans le réseau Wicri