L
L. A. Grishantseva
Researcher at National Research Nuclear University MEPhI
Publications - 58
Citations - 5547
L. A. Grishantseva is an academic researcher from National Research Nuclear University MEPhI. The author has contributed to research in topics: Cosmic ray & PAMELA detector. The author has an hindex of 16, co-authored 58 publications receiving 5320 citations.
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Journal ArticleDOI
An anomalous positron abundance in cosmic rays with energies 1.5-100 GeV
O. Adriani,G. C. Barbarino,G. A. Bazilevskaya,Roberto Bellotti,Mirko Boezio,E. A. Bogomolov,Lorenzo Bonechi,M. Bongi,V. Bonvicini,S. Bottai,A. Bruno,F. Cafagna,D. Campana,Per Carlson,Marco Casolino,G. Castellini,M. P. De Pascale,G. De Rosa,N. De Simone,V. Di Felice,A. M. Galper,L. A. Grishantseva,Petter Hofverberg,S. V. Koldashov,S. Y. Krutkov,A. N. Kvashnin,A. A. Leonov,V. Malvezzi,L. Marcelli,W. Menn,V. V. Mikhailov,E. Mocchiutti,Silvio Orsi,G. Osteria,P. Papini,Mark Pearce,P. Picozza,Marco Ricci,S. B. Ricciarini,M. Simon,Roberta Sparvoli,Piero Spillantini,Y. I. Stozhkov,Andrea Vacchi,E. Vannuccini,G. I. Vasilyev,S. A. Voronov,Y. T. Yurkin,G. Zampa,N. Zampa,V. G. Zverev +50 more
TL;DR: It is found that the positron fraction increases sharply over much of that range, in a way that appears to be completely inconsistent with secondary sources, and is concluded that a primary source, be it an astrophysical object or dark matter annihilation, is necessary.
Journal ArticleDOI
PAMELA Measurements of Cosmic-Ray Proton and Helium Spectra
O. Adriani,O. Adriani,G. C. Barbarino,G. A. Bazilevskaya,Roberto Bellotti,Mirko Boezio,E. A. Bogomolov,Lorenzo Bonechi,Lorenzo Bonechi,M. Bongi,V. Bonvicini,S. V. Borisov,S. Bottai,A. Bruno,F. Cafagna,D. Campana,R. Carbone,Per Carlson,Marco Casolino,G. Castellini,L. Consiglio,M. P. De Pascale,C. De Santis,N. De Simone,V. Di Felice,A. M. Galper,William Gillard,L. A. Grishantseva,Giovanna Jerse,A. V. Karelin,S. V. Koldashov,S. Y. Krutkov,A. N. Kvashnin,A. A. Leonov,V. V. Malakhov,V. Malvezzi,L. Marcelli,A. G. Mayorov,W. Menn,V. V. Mikhailov,E. Mocchiutti,Alfonso Monaco,Nicola Mori,Nicola Mori,N. N. Nikonov,G. Osteria,F. Palma,P. Papini,Mark Pearce,P. Picozza,C. Pizzolotto,Marco Ricci,S. B. Ricciarini,Laura Rossetto,Ritabrata Sarkar,M. Simon,Roberta Sparvoli,P. Spillantini,P. Spillantini,Y. I. Stozhkov,Andrea Vacchi,E. Vannuccini,G. I. Vasilyev,S. A. Voronov,Y. T. Yurkin,Juan Wu,G. Zampa,N. Zampa,V. G. Zverev +68 more
TL;DR: PAMELA data challenge the current paradigm of cosmic-ray acceleration in supernova remnants followed by diffusive propagation in the Galaxy and find that the spectral shapes of these two species are different and cannot be described well by a single power law.
Journal ArticleDOI
New measurement of the antiproton-to-proton flux ratio up to 100 GeV in the cosmic radiation.
O. Adriani,G. C. Barbarino,G. A. Bazilevskaya,Roberto Bellotti,Mirko Boezio,E. A. Bogomolov,Lorenzo Bonechi,M. Bongi,V. Bonvicini,S. Bottai,A. Bruno,F. Cafagna,D. Campana,P. Carlson,Marco Casolino,G. Castellini,M. P. De Pascale,G. De Rosa,D. Fedele,A. M. Galper,L. A. Grishantseva,Petter Hofverberg,A. A. Leonov,S. V. Koldashov,S. Y. Krutkov,A. N. Kvashnin,V. Malvezzi,L. Marcelli,W. Menn,V. V. Mikhailov,M. Minori,E. Mocchiutti,M. Nagni,S. Orsi,G. Osteria,P. Papini,Mark Pearce,P. Picozza,Marco Ricci,S. B. Ricciarini,M. Simon,Roberta Sparvoli,Piero Spillantini,Y. I. Stozhkov,E. Taddei,Andrea Vacchi,E. Vannuccini,G. I. Vasilyev,S. A. Voronov,Y. T. Yurkin,G. Zampa,N. Zampa,V. G. Zverev +52 more
TL;DR: A new measurement of the cosmic-ray antiproton-to-proton flux ratio between 1 and 100 GeV is presented, which is a tenfold improvement in statistics with respect to all previously published data.
Journal ArticleDOI
PAMELA results on the cosmic-ray antiproton flux from 60 MeV to 180 GeV in kinetic energy.
O. Adriani,G. C. Barbarino,G. A. Bazilevskaya,Roberto Bellotti,Mirko Boezio,E. A. Bogomolov,L. Bonechi,M. Bongi,V. Bonvicini,S. Borisov,S. Bottai,A. Bruno,F. Cafagna,D. Campana,R. Carbone,Per Carlson,Marco Casolino,G. Castellini,L. Consiglio,M. P. De Pascale,C. De Santis,N. De Simone,V. Di Felice,A. M. Galper,William Gillard,L. A. Grishantseva,Petter Hofverberg,Giovanna Jerse,A. V. Karelin,S. V. Koldashov,S. Y. Krutkov,A. N. Kvashnin,A. A. Leonov,V. Malvezzi,L. Marcelli,A. G. Mayorov,W. Menn,V. V. Mikhailov,E. Mocchiutti,Alfonso Monaco,Nicola Mori,N. N. Nikonov,G. Osteria,P. Papini,Mark Pearce,P. Picozza,C. Pizzolotto,Marco Ricci,S. B. Ricciarini,Laura Rossetto,M. Simon,Roberta Sparvoli,P. Spillantini,Y. I. Stozhkov,Andrea Vacchi,E. Vannuccini,G. I. Vasilyev,S. A. Voronov,Juan Wu,Y. T. Yurkin,G. Zampa,N. Zampa,V. G. Zverev +62 more
TL;DR: The satellite-borne experiment PAMELA has been used to make a new measurement of the cosmic-ray antiproton flux and the antipropton-to-proton flux ratio which extends previously published measurements down to 60 MeV and up to 180 GeV in kinetic energy.
Journal ArticleDOI
Cosmic-Ray Electron Flux Measured by the PAMELA Experiment between 1 and 625 GeV
O. Adriani,G. C. Barbarino,G. A. Bazilevskaya,Roberto Bellotti,Mirko Boezio,E. A. Bogomolov,M. Bongi,V. Bonvicini,S. V. Borisov,S. Bottai,A. Bruno,F. Cafagna,D. Campana,R. Carbone,P. Carlson,Marco Casolino,G. Castellini,L. Consiglio,M. P. De Pascale,C. De Santis,N. De Simone,V. Di Felice,A. M. Galper,William Gillard,L. A. Grishantseva,Giovanna Jerse,A. V. Karelin,S. V. Koldashov,S. Y. Krutkov,A. N. Kvashnin,A. A. Leonov,V. V. Malakhov,V. Malvezzi,L. Marcelli,A. G. Mayorov,W. Menn,V. V. Mikhailov,E. Mocchiutti,André Monaco,Nicola Mori,N. N. Nikonov,G. Osteria,F. Palma,P. Papini,Mark Pearce,P. Picozza,C. Pizzolotto,Marco Ricci,S. B. Ricciarini,Laura Rossetto,Ritabrata Sarkar,M. Simon,Roberta Sparvoli,Piero Spillantini,Steven Stochaj,J. C. Stockton,Y. I. Stozhkov,Andrea Vacchi,E. Vannuccini,G. I. Vasilyev,S. A. Voronov,Juan Wu,Y. T. Yurkin,G. Zampa,N. Zampa,V. G. Zverev +65 more
TL;DR: New results regarding negatively charged electrons between 1 and 625 GeV performed by the satellite-borne experiment PAMELA are presented, this is the first time that cosmic-ray e⁻ have been identified above 50 GeV.