The RS Oph outburst of 2021 monitored in X-rays with NICER

The 2021 outburst of the symbiotic recurrent nova RS Oph was monitored with the Neutron Star Interior Composition Explorer Mission (NICER) in the 0.2-12 keV range from day one after the optical maximum, until day 88, producing an unprecedented, detailed view of the outburst development. The X-ray flux preceding the supersoft X-ray phase peaked almost 5 days after optical maximum and originated only in shocked ejecta for 21 to 25 days. The emission was thermal; in the first 5 days only a non-collisional-ionization equilibrium model fits the spectrum, and a transition to equilibrium occurred between days 6 and 12. The ratio of peak X-rays flux measured in the NICER range to that measured with Fermi in the 60 MeV-500 GeV range was about 0.1, and the ratio to the peak flux measured with H.E.S.S. in the 250 GeV-2.5 TeV range was about 100. The central supersoft X-ray source (SSS), namely the shell hydrogen burning white dwarf (WD), became visible in the fourth week, initially with short flares. A huge increase in flux occurred on day 41, but the SSS flux remained variable. A quasi-periodic oscillation every ~35 s was always observed during the SSS phase, with variations in amplitude and a period drift that appeared to decrease in the end. The SSS has characteristics of a WD of mass >1 M(solar). Thermonuclear burning switched off shortly after day 75, earlier than in 2006 outburst. We discuss implications for the nova physics.Comment: Accepted for publication in the Astrophysical Journa

Voice control of smart home by using Google Cloud Speech-To-Text API

This work explains the process of creation two applications. The first application is an Android application that uses Speech-To-Text transcription by implementation of web service Google Speech API and Bluetooth communication as the client. The second application is a Windows application written in C# language using Bluetooth web service as the server. The applications show how Google Speech API works and how to implement these web services. The thesis consists of three main parts: Google Speech API, Bluetooth communication between the two devices, and the method to build an application using these features. The first part describes various ways to convert Speech into text form using Google Speech API and its features. It also explains what Speech to text conversion means and how this technique works. The second part describes the principle of operation of Bluetooth communication; how this communication works; how to implement Bluetooth service to a Windows application as the server and to an Android application as the client side. It also introduces its benefits but also its restrictions and its shortcomings. The third part deals with creating of the Windows and Android applications. This part describes how to implement these services to the specific applications, what is needed to set and how these applications work. The goal of the thesis has been met, both applications were created successfully and the whole system works correctly

The RS Oph Outburst of 2021 Monitored in X-Rays with NICER

Funder: Europe Regional Development Fund; Grant(s): ITMS2014+: 313011W085Abstract The 2021 outburst of the symbiotic recurrent nova RS Oph was monitored with the Neutron Star Interior Composition Explorer Mission (NICER) in the 0.2–12 keV range from day one after the optical maximum, until day 88, producing an unprecedented, detailed view of the outburst development. The X-ray flux preceding the supersoft X-ray phase peaked almost 5 days after optical maximum and originated only in shocked ejecta for 21–25 days. The emission was thermal; in the first 5 days, only a non-collisional-ionization equilibrium model fits the spectrum, and a transition to equilibrium occurred between days 6 and 12. The ratio of peak X-ray flux measured in the NICER range to that measured with Fermi in the 60 MeV–500 GeV range was about 0.1, and the ratio to the peak flux measured with H.E.S.S. in the 250 GeV–2.5 TeV range was about 100. The central supersoft X-ray source (SSS), namely the shell hydrogen burning white dwarf (WD), became visible in the fourth week, initially with short flares. A huge increase in flux occurred on day 41, but the SSS flux remained variable. A quasi-periodic oscillation every ≃35 s was always observed during the SSS phase, with variations in amplitude and a period drift that appeared to decrease in the end. The SSS has characteristics of a WD of mass &gt;1 M ⊙. Thermonuclear burning switched off shortly after day 75, earlier than in the 2006 outburst. We discuss implications for the nova physics.</jats:p

The RS Oph Outburst of 2021 Monitored in X-Rays with NICER

The 2021 outburst of the symbiotic recurrent nova RS Oph was monitored with the Neutron Star Interior Composition Explorer Mission (NICER) in the 0.2-12 keV range from day one after the optical maximum, until day 88, producing an unprecedented, detailed view of the outburst development. The X-ray flux preceding the supersoft X-ray phase peaked almost 5 days after optical maximum and originated only in shocked ejecta for 21-25 days. The emission was thermal; in the first 5 days, only a non-collisional-ionization equilibrium model fits the spectrum, and a transition to equilibrium occurred between days 6 and 12. The ratio of peak X-ray flux measured in the NICER range to that measured with Fermi in the 60 MeV-500 GeV range was about 0.1, and the ratio to the peak flux measured with H.E.S.S. in the 250 GeV-2.5 TeV range was about 100. The central supersoft X-ray source (SSS), namely the shell hydrogen burning white dwarf (WD), became visible in the fourth week, initially with short flares. A huge increase in flux occurred on day 41, but the SSS flux remained variable. A quasi-periodic oscillation every ≃35 s was always observed during the SSS phase, with variations in amplitude and a period drift that appeared to decrease in the end. The SSS has characteristics of a WD of mass >1 M ⊙. Thermonuclear burning switched off shortly after day 75, earlier than in the 2006 outburst. We discuss implications for the nova physics.Fil: Orio, Marina. Istituto Nazionale di Astrofisica; Italia. University of Wisconsin; Estados UnidosFil: Gendreau, Keith. Center for Exploration and Space Studies; Estados Unidos. National Aeronautics and Space Administration; Estados UnidosFil: Giese, Morgan. University of Wisconsin; Estados UnidosFil: Luna, Gerardo Juan Manuel. Universidad de Buenos Aires; Argentina. Universidad Nacional de Hurlingham; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas; ArgentinaFil: Magdolen, Jozef. Slovak University of Technology in Bratislava; EslovaquiaFil: Strohmayer, Tod E.. National Aeronautics and Space Administration; Estados UnidosFil: Zhang, Andy E.. University of Wisconsin; Estados UnidosFil: Altamirano, Diego. University of Southampton; Reino UnidoFil: Dobrotka, Andrej. Slovak University of Technology in Bratislava; EslovaquiaFil: Enoto, Teruaki. Riken Cluster For Pioneering Research; JapónFil: Ferrara, Elizabeth C.. University of Maryland; Estados Unidos. National Aeronautics and Space Administration; Estados UnidosFil: Ignace, Richard. East Tennessee State University; Estados UnidosFil: Heinz, Sebastian. University of Wisconsin; Estados UnidosFil: Markwardt, Craig. National Aeronautics and Space Administration; Estados UnidosFil: Nichols, Joy S.. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Parker, Michael L.. University of Cambridge; Estados UnidosFil: Pasham, Dheeraj R.. Mit Kavli Institute For Astrophysics And Space Research; Estados UnidosFil: Pei, Songpeng. Liupanshui Normal University; ChinaFil: Pradhan, Pragati. Embry-riddle Aeronautical University, Prescott; China. Mit Kavli Institute For Astrophysics And Space Research; Estados UnidosFil: Remillard, Ron. Mit Kavli Institute For Astrophysics And Space Research; Estados UnidosFil: Steiner, James F.. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Tombesi, Francesco. University of Maryland; Estados Unidos. Universita Tor Vergata; Italia. National Aeronautics and Space Administration; Estados Unido

The RS Oph Outburst of 2021 Monitored in X-Rays with NICER

The 2021 outburst of the symbiotic recurrent nova RS Oph was monitored with the Neutron Star Interior Composition Explorer Mission (NICER) in the 0.2–12 keV range from day one after the optical maximum, until day 88, producing an unprecedented, detailed view of the outburst development. The X-ray flux preceding the supersoft X-ray phase peaked almost 5 days after optical maximum and originated only in shocked ejecta for 21–25 days. The emission was thermal; in the first 5 days, only a non-collisional-ionization equilibrium model fits the spectrum, and a transition to equilibrium occurred between days 6 and 12. The ratio of peak X-ray flux measured in the NICER range to that measured with Fermi in the 60 MeV–500 GeV range was about 0.1, and the ratio to the peak flux measured with H.E.S.S. in the 250 GeV–2.5 TeV range was about 100. The central supersoft X-ray source (SSS), namely the shell hydrogen burning white dwarf (WD), became visible in the fourth week, initially with short flares. A huge increase in flux occurred on day 41, but the SSS flux remained variable. A quasi-periodic oscillation every ≃35 s was always observed during the SSS phase, with variations in amplitude and a period drift that appeared to decrease in the end. The SSS has characteristics of a WD of mass >1 M _⊙ . Thermonuclear burning switched off shortly after day 75, earlier than in the 2006 outburst. We discuss implications for the nova physics

The RS Oph outburst of 2021 monitored in x-rays with NICER

The 2021 outburst of the symbiotic recurrent nova RS Oph was monitored with the Neutron Star Interior Composition Explorer Mission (NICER) in the 0.2–12 keV range from day one after the optical maximum, until day 88, producing an unprecedented, detailed view of the outburst development. The X-ray flux preceding the supersoft X-ray phase peaked almost 5 days after optical maximum and originated only in shocked ejecta for 21–25 days. The emission was thermal; in the first 5 days, only a non-collisional-ionization equilibrium model fits the spectrum, and a transition to equilibrium occurred between days 6 and 12. The ratio of peak X-ray flux measured in the NICER range to that measured with Fermi in the 60 MeV–500 GeV range was about 0.1, and the ratio to the peak flux measured with H.E.S.S. in the 250 GeV–2.5 TeV range was about 100. The central supersoft X-ray source (SSS), namely the shell hydrogen burning white dwarf (WD), became visible in the fourth week, initially with short flares. A huge increase in flux occurred on day 41, but the SSS flux remained variable. A quasi-periodic oscillation every ≃35 s was always observed during the SSS phase, with variations in amplitude and a period drift that appeared to decrease in the end. The SSS has characteristics of a WD of mass &gt;1 M⊙. Thermonuclear burning switched off shortly after day 75, earlier than in the 2006 outburst. We discuss implications for the nova physics