Proyecto de Investigación: ESTUDIO MULTIDISCIPLINAR DE PROCESOS ALTAMENTE ENERGETICOS EN EYECCIONES ASTROFISICAS: TEORIA Y OBSERVACIONES
Cargando...
Colaboradores
Financiadores
ID
AYA2016-76012-C3-1-P
Autores
Publicaciones
Observatory science with eXTP
(Springer Link, 2018-08-30) Zand, J. J. M.; Bozzo, E.; Qu, J.; Li, X. D.; Amati, L.; Chen, Y.; Donnarumma, I.; Doroshenko, V.; Drake, S. A.; Hernanz, M.; Jenke, P. A.; Baykal, A.; Cumming, A.; Miller, M. C.; Gendre, B.; McHardy, I.; Peretz, U.; Schatz, H.; Brown, E. F.; Neubert, T.; Gill, R.; Mikusincova, R.; Prescod Weinstein, C.; Shearer, A.; Campana, R.; Pacciani, L.; Götz, D.; Rodríguez, J.; Stappers, B. W.; Chambers, F.; Paul, B.; Gouiffès, C.; Rózanska, A.; Strohmayer, T. E.; Chenevez, J.; De Martino, D.; Malzac, J.; Suleimanov, V. F.; Ciolfi, R.; Tauris, T. M.; Méndez, M.; Svoboda, J.; D´aì, A.; Atteia, J. L.; Motch, C.; Thielemann, F. K.; D´Ammando, F.; Mahmoodifar, S.; Tombesi, F.; Degenaar, N.; Zingale, M.; Torres, D. F.; D´Elia, V.; Zhang, S.; Torresi, E.; Doyle, G.; Zhang, S. N.; Fan, X.; Zdziarski, A. A.; Malyshev, D.; Zane, S.; Maccarone, Thomas J.; Zampieri, L.; Zhang, X.; Yuan, F.; Stratta, G.; Yu, W.; Younes, G.; Yan, Z.; Xu, Y.; Xiong, S. L.; Sala, G.; Agudo, I.; Ballantyne, D. R.; Bianchi, S.; Brandt, S.; Cackett, E. M.; Grandi, P.; Granot, J.; Güdel, M.; Heger, A.; Heinke, C. O.; Homan, J.; Iaria, R.; Iwasawa, K.; Izzo, L.; Ji, L.; Del Santo, M.; De Pasquale, M.; Dai, Z. G.; Constantin, E.; Chernyakova, M.; Chen, L.; Casella, P.; Burderi, L.; Braga, J.; Belloni, T.; Andersson, N. A.; Osborne, Julian P.; Wilms, J.; Nardini, E.; De Rosa, A.; Behar, E.; Turriziani, S.; Altamirano, D.; Cavecchi, Y.; Di Salvo, T.; Papadakis, L. E.; Blay, P.; Vacchi, A.; Chen, Y. P.; Falanga, M.; Pérez Torres, M. A.; Bucciantini, N.; Vercellone, S.; Jin, C. C.; Ferdman, R. D.; Reig, P.; Campana, S.; Rowlinson, A.; Feroci, M.; Rodríguez Gil, P.; Lu., F.; Zhou, P.; Fraschetti, F.; Sakamoto, T.; Mehdipour, M.; Baglio, C.; Galloway, D. K.; Salvaterra, R.; Bhattacharyya, S.; Gambino, A. F.; Santagelo, A.; Longo, F.; Gandhi, P.; Schanne, S.; Liang, E. W.; Ge, M.; Shao, L.; Kunneriath, D.; Shore, S. N.; Kuiper, L.; Rossi, E. M.; Kreykenbohm, I.; Wu, X.; Komossa, S.; Linares, M.; Keek, L.; Li, G.; Kawai, N.; Kargaltsev, O.; Kalemci, E.; Kaastra, J. S.; José, J.; Jonker, P. G.; Manousakis, A.; Mignani, R. P.; Nättilä, J.; Orlandini, M.; Paolillo, M.; Vink, J. S.; Wang, J. J.; Wang, J. F.; Watts, A. L.; Weng, S.; Weinberg, N. N.; Wheatley, P. J.; Wijnands, R.; Woods, T. E.; Woosley, S. E.; Savolainen, T.; Sanna, A.; Salmi, T.; Romano, P.; Riggio, A.; Perinati, E.; Pellizzoni, A.; Paltani, Stéphane; O´Brien, P. T.; Miniutti, G.; Men, Y.; Bilous, A.; Lutovinov, A. A.; National Natural Science Foundation of China (NSFC); European Research Council (ERC); National Aeronautics and Space Administration (NASA); Agencia Estatal de Investigación (AEI); Royal Society; Strategic Priority Research Program of the Chinese Academy of Sciences; European Research Council (ERC); National Science Centre, Poland (NCN); Unidad de Excelencia Científica María de Maeztu Instituto de Ciencias del Cosmos (ICCUB), MDM-2014-0369
In this White Paper we present the potential of the enhanced X-ray Timing and Polarimetry (eXTP) mission for studies related to Observatory Science targets. These include flaring stars, supernova remnants, accreting white dwarfs, low and high mass X-ray binaries, radio quiet and radio loud active galactic nuclei, tidal disruption events, and gamma-ray bursts. eXTP will be excellently suited to study one common aspect of these objects: their often transient nature. Developed by an international Consortium led by the Institute of High Energy Physics of the Chinese Academy of Science, the eXTP mission is expected to be launched in the mid 2020s.
The quest for dual and binary supermassive black holes: A multi-messenger view
(Elsevier BV, 2019-12-12) De Rosa, A.; Vignali, C.; Bogdanovic, T.; Capelo, P. R.; Charisi, M.; Dotti, M.; Husemann, B.; Lusso, E.; Mayer, L.; Paragi, Z.; Runnoe, J.; Sesana, A.; Steinborn, L.; Bianchi, S.; Colpi, M.; Del Valle, L.; Frey, S.; Gabányi, K. É.; Giustini, M.; Guainazzi, M.; Haiman, Z.; Herrera Ruiz, N.; Herrero Illana, R.; Iwasawa, K.; Komossa, S.; Lena, D.; Loiseau, N.; Pérez Torres, M.; Piconcelli, E.; Volonteri, M.; Agenzia Spaziale Italiana (ASI); Istituto Nazionale Astrofisica (INAF); National Aeronautics and Space Administration (NASA); Hungarian Scientific Research Fund (OTKA); Hungarian Academy of Sciences (MTA); Deutsche Forschungsgemeinschaft (DFG); European Union COFUND/Durham Junior Research Fellowship (EU); European Research Council (ERC); Swiss National Science Foundation (SNSF); Federal Ministry of Education & Research (BMBF); Ministerio de Economía y Competitividad (MINECO); Comunidad de Madrid; Agencia Estatal de Investigación (AEI); Lena, D. [0000-0003-4184-6152]; Loiseau, N. [0000-0001-5471-3776]; Haiman, Z. [0000-0003-3633-5403]; De Rosa, A. [0000-0001-5668-6863]; Husemann, B. [0000-0003-2901-6842]; Centros de Excelencia Severo Ochoa, INSTITUTO DE ASTROFISICA DE ANDALUCIA (IAA), SEV-2017-0709; Unidad de Excelencia Científica María de Maeztu Instituto de Ciencias del Cosmos (ICCUB), MDM-2014-0369; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737
The quest for binary and dual supermassive black holes (SMBHs) at the dawn of the multi-messenger era is compelling. Detecting dual active galactic nuclei (AGN) - active SMBHs at projected separations larger than several parsecs - and binary AGN - probing the scale where SMBHs are bound in a Keplerian binary - is an observational challenge. The study of AGN pairs (either dual or binary) also represents an overarching theoretical problem in cosmology and astrophysics. The AGN triggering calls for detailed knowledge of the hydrodynamical conditions of gas in the imminent surroundings of the SMBHs and, at the same time, their duality calls for detailed knowledge on how galaxies assemble through major and minor mergers and grow fed by matter along the filaments of the cosmic web. This review describes the techniques used across the electromagnetic spectrum to detect dual and binary AGN candidates and proposes new avenues for their search. The current observational status is compared with the state-of-the-art numerical simulations and models for formation of dual and binary AGN. Binary SMBHs are among the loudest sources of gravitational waves (GWs) in the Universe. The search for a background of GWs at nHz frequencies from inspiralling SMBHs at low redshifts, and the direct detection of signals from their coalescence by the Laser Interferometer Space Antenna in the next decade, make this a theme of major interest for multi-messenger astrophysics. This review discusses the future facilities and observational strategies that are likely to significantly advance this fascinating field.
The high-energy emission from HD 93129A near periastron
(Oxford Academics: Oxford University Press, 2020-05-05) Del Palacio, S.; García, F.; Altamirano, D.; Barbá, R. H.; Bosch Ramon, V.; Corcoran, M.; De Becker, M.; Hamaguchi, K.; Maíz Apellániz, J.; Munar Adrover, P.; Paredes, J. M.; Romero, G. E.; Sana, H.; Tavani, M.; Ud Doula, A.; Agencia Estatal de Investigación (AEI); Consejo Nacional de Investigaciones Científicas y Técnicas (CONICET); Dutch Research Council (NWO); García, F. [0000-0001-9072-4069]; Altamirano, D. [0000-0002-3422-0074]; Barbá, R. [0000-0003-1086-1579]; Corcoran, M. [0000-0002-7762-3172]; Del Palacio, S. [0000-0002-5761-2417]; Unidad de Excelencia Científica María de Maeztu Instituto de Ciencias del Cosmos (ICCUB), MDM-2014-0369; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737
We conducted an observational campaign towards one of the most massive and luminous colliding wind binaries in the Galaxy, HD 93129A, close to its periastron passage in 2018. During this time the source was predicted to be in its maximum of high-energy emission. Here we present our data analysis from the X-ray satellites Chandra and NuSTAR and the γ-ray satellite AGILE. High-energy emission coincident with HD 93129A was detected in the X-ray band up to ∼18 keV, whereas in the γ-ray band only upper limits were obtained. We interpret the derived fluxes using a non-thermal radiative model for the wind-collision region. We establish a conservative upper limit for the fraction of the wind kinetic power that is converted into relativistic electron acceleration, fNT,e < 0.02. In addition, we set a lower limit for the magnetic field in the wind-collision region as BWCR > 0.3 G. We also argue a putative interpretation of the emission from which we estimate fNT,e ≈ 0.006 and BWCR ≈ 0.5 G. We conclude that multiwavelength, dedicated observing campaigns during carefully selected epochs are a powerful tool for characterizing the relativistic particle content and magnetic field intensity in colliding wind binaries.
