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(PDF) Accretion-Ejection Mechanism of Cygnus X-3 | Manojendu Choudhury - Academia.edu
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Supplement</p><div class="ds-work-card--button-container"><button class="ds2-5-button js-swp-download-button" data-signup-modal="{"location":"continue-reading-button--work-card","attachmentId":108406071,"attachmentType":"pdf","workUrl":"https://www.academia.edu/110656229/Accretion_Ejection_Mechanism_of_Cygnus_X_3"}">See full PDF</button><button class="ds2-5-button ds2-5-button--secondary js-swp-download-button" data-signup-modal="{"location":"download-pdf-button--work-card","attachmentId":108406071,"attachmentType":"pdf","workUrl":"https://www.academia.edu/110656229/Accretion_Ejection_Mechanism_of_Cygnus_X_3"}"><span class="material-symbols-outlined" style="font-size: 20px" translate="no">download</span>Download PDF</button></div></div></div></div><div data-auto_select="false" data-client_id="331998490334-rsn3chp12mbkiqhl6e7lu2q0mlbu0f1b" data-doc_id="108406071" data-landing_url="https://www.academia.edu/110656229/Accretion_Ejection_Mechanism_of_Cygnus_X_3" data-login_uri="https://www.academia.edu/registrations/google_one_tap" data-moment_callback="onGoogleOneTapEvent" id="g_id_onload"></div><div class="ds-top-related-works--grid-container"><div class="ds-related-content--container ds-top-related-works--container"><h2 class="ds-related-content--heading">Related papers</h2><div class="ds-related-work--container js-wsj-grid-card" data-collection-position="0" data-entity-id="70666673" data-sort-order="default"><a class="ds-related-work--title js-wsj-grid-card-title ds2-5-body-md ds2-5-body-link" href="https://www.academia.edu/70666673/Clumpy_Wind_Accretion_in_Cygnus_X_1">Clumpy Wind Accretion in Cygnus X-1</a><div class="ds-related-work--metadata"><a class="js-wsj-grid-card-author ds2-5-body-sm ds2-5-body-link" data-author-id="179606654" href="https://uw.academia.edu/IshikaPalit">Ishika Palit</a></div><p class="ds-related-work--metadata ds2-5-body-xs">arXiv: High Energy Astrophysical Phenomena, 2020</p><p class="ds-related-work--abstract ds2-5-body-sm">Cygnus X-1 is one of the brightest X-ray sources observed and shows the X-ray intensity variations on time scales from milliseconds to months in both the soft and hard X-rays. The accretion onto the black hole is believed to be wind fed due to focused stellar wind from the binary companion HDE-226868. We aim to understand the physical mechanism responsible for the short timescale X-ray variability ($&lt;$100 s) of the source in its Hard/Low state. We compute the 2D relativistic hydrodynamic simulation of the low angular momentum accretion flow with a time dependent outer boundary condition that reflects the focused, clumpy wind from the super-giant in this X-ray binary system. We follow the dynamical evolution of our model for about 100 s and present the results showing an oscillatory shock, being a potential explanation of variability observed in hard X-rays. 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From the decay timescale of the Balmer emission associated with the nebula we measure an outflow mass M_wind 4x10^-6 Msun. Remarkably, this is 100 times larger than the accreted mass and 10 The wind efficiency must therefore be significantly larger than previous estimates for black hole transients, suggesting that radiation pressure (in addition to other mechanisms such as Compton-heating) plays a key role in V404 Cyg. In addition, we compare the evolution of the 2015 and 1989 outbursts and find clear similarities (namely a large luminosity drop 10 d after the X-ray trigger, followed by a brief nebular phase) but also remarkable differences in decay timescales and long-term evolution of the Halpha profile. In particular, we see evidence for a rapid disc contraction in 2015, consistent with a burst of mass transfer. This could be driven b...</p><div class="ds-related-work--ctas"><button class="ds2-5-text-link ds2-5-text-link--inline js-swp-download-button" data-signup-modal="{"location":"wsj-grid-card-download-pdf-modal","work_title":"Accretion and Outflow in V404 Cyg","attachmentId":82017288,"attachmentType":"pdf","work_url":"https://www.academia.edu/73530077/Accretion_and_Outflow_in_V404_Cyg","alternativeTracking":true}"><span class="material-symbols-outlined" style="font-size: 18px" translate="no">download</span><span class="ds2-5-text-link__content">Download free PDF</span></button><a class="ds2-5-text-link ds2-5-text-link--inline js-wsj-grid-card-view-pdf" href="https://www.academia.edu/73530077/Accretion_and_Outflow_in_V404_Cyg"><span class="ds2-5-text-link__content">View PDF</span><span class="material-symbols-outlined" style="font-size: 18px" translate="no">chevron_right</span></a></div></div><div class="ds-related-work--container js-wsj-grid-card" data-collection-position="2" data-entity-id="21964889" data-sort-order="default"><a class="ds-related-work--title js-wsj-grid-card-title ds2-5-body-md ds2-5-body-link" href="https://www.academia.edu/21964889/A_transient_relativistic_radio_jet_from_Cygnus_X_1">A transient relativistic radio jet from Cygnus X-1</a><div class="ds-related-work--metadata"><a class="js-wsj-grid-card-author ds2-5-body-sm ds2-5-body-link" data-author-id="43161102" href="https://independent.academia.edu/GuyPooley">Guy Pooley</a></div><p class="ds-related-work--metadata ds2-5-body-xs">Monthly Notices of the Royal Astronomical Society, 2006</p><div class="ds-related-work--ctas"><button class="ds2-5-text-link ds2-5-text-link--inline js-swp-download-button" data-signup-modal="{"location":"wsj-grid-card-download-pdf-modal","work_title":"A transient relativistic radio jet from Cygnus X-1","attachmentId":42680964,"attachmentType":"pdf","work_url":"https://www.academia.edu/21964889/A_transient_relativistic_radio_jet_from_Cygnus_X_1","alternativeTracking":true}"><span class="material-symbols-outlined" style="font-size: 18px" translate="no">download</span><span class="ds2-5-text-link__content">Download free PDF</span></button><a class="ds2-5-text-link ds2-5-text-link--inline js-wsj-grid-card-view-pdf" href="https://www.academia.edu/21964889/A_transient_relativistic_radio_jet_from_Cygnus_X_1"><span class="ds2-5-text-link__content">View PDF</span><span class="material-symbols-outlined" style="font-size: 18px" translate="no">chevron_right</span></a></div></div><div class="ds-related-work--container js-wsj-grid-card" data-collection-position="3" data-entity-id="64842783" data-sort-order="default"><a class="ds-related-work--title js-wsj-grid-card-title ds2-5-body-md ds2-5-body-link" href="https://www.academia.edu/64842783/Cygnus_X_3_Its_Little_Friend_s_Counterpart_the_Distance_to_Cygnus_X_3_and_Outflows_Jets">Cygnus X-3: Its Little Friend’s Counterpart, the Distance to Cygnus X-3, and Outflows/Jets</a><div class="ds-related-work--metadata"><a class="js-wsj-grid-card-author ds2-5-body-sm ds2-5-body-link" data-author-id="38792048" href="https://independent.academia.edu/MichaelMcCollough">Michael McCollough</a></div><p class="ds-related-work--metadata ds2-5-body-xs">The Astrophysical Journal, 2016</p><div class="ds-related-work--ctas"><button class="ds2-5-text-link ds2-5-text-link--inline js-swp-download-button" data-signup-modal="{"location":"wsj-grid-card-download-pdf-modal","work_title":"Cygnus X-3: Its Little Friend’s Counterpart, the Distance to Cygnus X-3, and 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href="https://www.academia.edu/57871384/Transient_gamma_ray_emission_from_Cygnus_X_3">Transient gamma-ray emission from Cygnus X-3</a><div class="ds-related-work--metadata"><a class="js-wsj-grid-card-author ds2-5-body-sm ds2-5-body-link" data-author-id="13356590" href="https://unlp.academia.edu/GustavoRomero">Gustavo E Romero</a></div><p class="ds-related-work--metadata ds2-5-body-xs">Proceedings of 25th Texas Symposium on Relativistic Astrophysics — PoS(Texas 2010)</p><div class="ds-related-work--ctas"><button class="ds2-5-text-link ds2-5-text-link--inline js-swp-download-button" data-signup-modal="{"location":"wsj-grid-card-download-pdf-modal","work_title":"Transient gamma-ray emission from Cygnus X-3","attachmentId":72558300,"attachmentType":"pdf","work_url":"https://www.academia.edu/57871384/Transient_gamma_ray_emission_from_Cygnus_X_3","alternativeTracking":true}"><span class="material-symbols-outlined" style="font-size: 18px" translate="no">download</span><span class="ds2-5-text-link__content">Download free PDF</span></button><a class="ds2-5-text-link ds2-5-text-link--inline js-wsj-grid-card-view-pdf" href="https://www.academia.edu/57871384/Transient_gamma_ray_emission_from_Cygnus_X_3"><span class="ds2-5-text-link__content">View PDF</span><span class="material-symbols-outlined" style="font-size: 18px" translate="no">chevron_right</span></a></div></div><div class="ds-related-work--container js-wsj-grid-card" data-collection-position="5" data-entity-id="94098881" data-sort-order="default"><a class="ds-related-work--title js-wsj-grid-card-title ds2-5-body-md ds2-5-body-link" href="https://www.academia.edu/94098881/Accretion_disk_and_stream_origin_of_the_dip_phenomenon_in_Hercules_X_1">Accretion disk and stream origin of the dip phenomenon in Hercules X-1</a><div class="ds-related-work--metadata"><a class="js-wsj-grid-card-author ds2-5-body-sm ds2-5-body-link" data-author-id="239013121" href="https://independent.academia.edu/LeahyDenis">Denis Leahy</a></div><p class="ds-related-work--metadata ds2-5-body-xs">Proceedings of the International Astronomical Union, 2012</p><p class="ds-related-work--abstract ds2-5-body-sm">The Rossi X-ray Timing Explorer has observed Hercules X-1 over a period of about 13 years, allowing detailed measurement of the properties of the dip phenomenon. We construct a model for the dips based on the impact between the accretion stream and the disk, including the geometry and dynamics of the stream and disk. We also consider the case where the stream penetrates the outer parts of the disk, where its density is low, and proceeds to a second impact at smaller radius in the disk. The results from the model are discussed and compared to the observed properties of the dips.</p><div class="ds-related-work--ctas"><button class="ds2-5-text-link ds2-5-text-link--inline js-swp-download-button" data-signup-modal="{"location":"wsj-grid-card-download-pdf-modal","work_title":"Accretion disk and stream origin of the dip phenomenon in Hercules X-1","attachmentId":96652106,"attachmentType":"pdf","work_url":"https://www.academia.edu/94098881/Accretion_disk_and_stream_origin_of_the_dip_phenomenon_in_Hercules_X_1","alternativeTracking":true}"><span class="material-symbols-outlined" style="font-size: 18px" translate="no">download</span><span class="ds2-5-text-link__content">Download free PDF</span></button><a class="ds2-5-text-link ds2-5-text-link--inline js-wsj-grid-card-view-pdf" href="https://www.academia.edu/94098881/Accretion_disk_and_stream_origin_of_the_dip_phenomenon_in_Hercules_X_1"><span class="ds2-5-text-link__content">View PDF</span><span class="material-symbols-outlined" style="font-size: 18px" translate="no">chevron_right</span></a></div></div><div class="ds-related-work--container js-wsj-grid-card" data-collection-position="6" data-entity-id="8885341" data-sort-order="default"><a class="ds-related-work--title js-wsj-grid-card-title ds2-5-body-md ds2-5-body-link" href="https://www.academia.edu/8885341/Accretion_mode_changes_in_Centaurus_X_3">Accretion mode changes in Centaurus X-3</a><div class="ds-related-work--metadata"><a class="js-wsj-grid-card-author ds2-5-body-sm ds2-5-body-link" data-author-id="19499579" href="https://independent.academia.edu/BiswajitPaul16">Biswajit Paul</a></div><p class="ds-related-work--metadata ds2-5-body-xs">Astronomy & Astrophysics, 2005</p><p class="ds-related-work--abstract ds2-5-body-sm">We report here discovery of the existence of two different accretion modes in the high mass X-ray binary pulsar Cen X-3 during its high states. The multiband X-ray light curves of Cen X-3 lasting for more than 3400 days obtained with the All Sky Monitor (ASM) onboard the Rossi X-ray Timing Explorer (RXTE) shows many episodes of high and low X-ray intensities. The high intensity phases last between a few to upto 110 days and the separation between two high intensity phases also varies widely. One remarkable feature deduced from the RXTE-ASM light curves is that during these high intensity phases, Cen X-3 manifests in two very distinct spectral states. When the source makes a transition from the low intensity phase to the high intensity phase, it adopts one of these two spectral states and during the entire high intensity phase remains in that particular spectral state. During December 2000 to April 2004, all the high intensity episodes showed a hardness ratio which is significantly larger than the same during all the high states prior to and subsequent to this period. It is also found that most of the soft outbursts reach a nearly constant peak flux in the 5--12 keV band. For comparison, similar analysis was carried out on the long term X-ray light curves of three other X-ray binary pulsars Her X-1, Vela X-1, and SMC X-1. Results obtained with these sources are also presented here and we found that none of the other sources show such a behaviour. From these observations, we suggest that Cen X-3 has two different accretion modes and in the course of nine years it has exhibited two switch overs between these.</p><div class="ds-related-work--ctas"><button class="ds2-5-text-link ds2-5-text-link--inline js-swp-download-button" data-signup-modal="{"location":"wsj-grid-card-download-pdf-modal","work_title":"Accretion mode changes in Centaurus X-3","attachmentId":35217261,"attachmentType":"pdf","work_url":"https://www.academia.edu/8885341/Accretion_mode_changes_in_Centaurus_X_3","alternativeTracking":true}"><span class="material-symbols-outlined" style="font-size: 18px" translate="no">download</span><span class="ds2-5-text-link__content">Download free PDF</span></button><a class="ds2-5-text-link ds2-5-text-link--inline js-wsj-grid-card-view-pdf" href="https://www.academia.edu/8885341/Accretion_mode_changes_in_Centaurus_X_3"><span class="ds2-5-text-link__content">View PDF</span><span class="material-symbols-outlined" style="font-size: 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