From davide.gizzi at astro.su.se Thu Jan 20 15:04:26 2022 From: davide.gizzi at astro.su.se (Davide Gizzi) Date: Thu, 20 Jan 2022 14:04:26 +0000 Subject: [Okc-wp4] EO meeting: 27th of January Message-ID: Dear all, our first EO meeting of the year will take place on Thursday, 27th of January, at 13:15 (CET). The speaker is Aurore Betranhandy, PhD student in her final year of study, working with prof. Evan O'Connor on simulations of core-collapse supernovae explosions. Aurore has recently got a postdoc position at the Albert Einstein Institute in Potsdam, where she is going to work with prof. Masaru Shibata. To join the meeting: https://stockholmuniversity.zoom.us/j/65883589027?pwd=RGxJOUVQWmNtMlZFMUIwaHRabkExdz09 Meeting ID: 658 8358 9027 Below is title and abstract of the talk. Title: Axion emission impact on Core-Collapse Supernovae simulations Abstract: Core-Collapse Supernovae (CCSNe) are some of the most important phenomenon in the Universe, from their impact on the nucleosynthesis to being the birth place of neutron stars. However, the exact mechanisms behind the final explosion is still unobserved and we have to rely on simulations to try and understand them. Axions have been suggested as being important particles in CCSN simulations due to their impact on the proto-neutron star cooling. In this talk I will explain how we did include axion emission in our simulation code FLASH and then present our latest results with 1D and 2D simulations showing the impact of said inclusion. Hope to see you there! Ana Sagués Carracedo & Davide Gizzi -------------- next part -------------- An HTML attachment was scrubbed... URL: From davide.gizzi at astro.su.se Thu Jan 27 08:00:52 2022 From: davide.gizzi at astro.su.se (Davide Gizzi) Date: Thu, 27 Jan 2022 07:00:52 +0000 Subject: [Okc-wp4] EO meeting: 27th of January In-Reply-To: References: Message-ID: <7ed528fb93f244b1aa3b50b762a9c891@astro.su.se> Dear all, a kind reminder of the EO meeting today at 13:15 (CET). Kind regards ________________________________ From: Davide Gizzi Sent: Thursday, January 20, 2022 3:04:26 PM To: Okc-wp4 at fysik.su.se; people at nordita.org Cc: Aurore Michele Marie Betranhandy Subject: EO meeting: 27th of January Dear all, our first EO meeting of the year will take place on Thursday, 27th of January, at 13:15 (CET). The speaker is Aurore Betranhandy, PhD student in her final year of study, working with prof. Evan O'Connor on simulations of core-collapse supernovae explosions. Aurore has recently got a postdoc position at the Albert Einstein Institute in Potsdam, where she is going to work with prof. Masaru Shibata. To join the meeting: https://stockholmuniversity.zoom.us/j/65883589027?pwd=RGxJOUVQWmNtMlZFMUIwaHRabkExdz09 Meeting ID: 658 8358 9027 Below is title and abstract of the talk. Title: Axion emission impact on Core-Collapse Supernovae simulations Abstract: Core-Collapse Supernovae (CCSNe) are some of the most important phenomenon in the Universe, from their impact on the nucleosynthesis to being the birth place of neutron stars. However, the exact mechanisms behind the final explosion is still unobserved and we have to rely on simulations to try and understand them. Axions have been suggested as being important particles in CCSN simulations due to their impact on the proto-neutron star cooling. In this talk I will explain how we did include axion emission in our simulation code FLASH and then present our latest results with 1D and 2D simulations showing the impact of said inclusion. Hope to see you there! Ana Sagués Carracedo & Davide Gizzi -------------- next part -------------- An HTML attachment was scrubbed... URL: From davide.gizzi at astro.su.se Thu Feb 3 10:27:11 2022 From: davide.gizzi at astro.su.se (Davide Gizzi) Date: Thu, 3 Feb 2022 09:27:11 +0000 Subject: [Okc-wp4] EO meeting: 10th of February Message-ID: <2d9accb3066d43489d1f1566d191f015@astro.su.se> Dear all, our next EO meeting will take place on Thursday, 10th of February, at 13:15 (CET). The speaker is Quentin Pognan, PhD student of Anders Jerkstrand (Stockholm University), working on light curves and spectra of kilonovae. He is going to talk about his recent work on this topic. To join the meeting: https://stockholmuniversity.zoom.us/j/65883589027?pwd=RGxJOUVQWmNtMlZFMUIwaHRabkExdz09 Meeting ID: 658 8358 9027 Below is title and abstract of the talk. Title: The validity of the LTE and steady-state approximations for nebular phase kilonovae Abstract: Kilonovae (KN) following a binary neutron star merger are expected to enter a non-local thermodynamic equilibrium (NLTE) regime several days after merger, as ejecta densities rapidly fall. Accompanying this transition away from local thermodynamic equilibrium (LTE), is a transition to a ‘nebular’ phase, where spectra are dominated by emission lines, as opposed to scattering lines over a quasi-blackbody continuum. The nebular phase is initially in a ‘steady-state’ regime, until thermal reprocessing timescales become long, at which point the temperature and ionization states need to be evolved time-dependently. Since nebular phase spectra offer a possibility of element identification in KN, it is interesting to study the onset and significance of time-dependent effects. I will present a study into these effects conducted using the spectral synthesis code SUMO, and demonstrate that time-dependent calculations may be necessary for certain ejecta parameters. I will also briefly present some ongoing work on the importance of NLTE calculations for post-peak KN, with a focus on consequences for expansion opacities. Hope to see you there! Ana Sagués Carracedo & Davide Gizzi -------------- next part -------------- An HTML attachment was scrubbed... URL: From davide.gizzi at astro.su.se Thu Feb 10 07:34:00 2022 From: davide.gizzi at astro.su.se (Davide Gizzi) Date: Thu, 10 Feb 2022 06:34:00 +0000 Subject: [Okc-wp4] EO meeting: 10th of February In-Reply-To: <2d9accb3066d43489d1f1566d191f015@astro.su.se> References: <2d9accb3066d43489d1f1566d191f015@astro.su.se> Message-ID: Dear all, a kind reminder of today's EO meeting. Kind regards ________________________________ From: Davide Gizzi Sent: Thursday, February 3, 2022 10:27:11 AM To: Okc-wp4 at fysik.su.se; people at nordita.org Cc: Quentin Perceval Xavier Pognan Subject: EO meeting: 10th of February Dear all, our next EO meeting will take place on Thursday, 10th of February, at 13:15 (CET). The speaker is Quentin Pognan, PhD student of Anders Jerkstrand (Stockholm University), working on light curves and spectra of kilonovae. He is going to talk about his recent work on this topic. To join the meeting: https://stockholmuniversity.zoom.us/j/65883589027?pwd=RGxJOUVQWmNtMlZFMUIwaHRabkExdz09 Meeting ID: 658 8358 9027 Below is title and abstract of the talk. Title: The validity of the LTE and steady-state approximations for nebular phase kilonovae Abstract: Kilonovae (KN) following a binary neutron star merger are expected to enter a non-local thermodynamic equilibrium (NLTE) regime several days after merger, as ejecta densities rapidly fall. Accompanying this transition away from local thermodynamic equilibrium (LTE), is a transition to a ‘nebular’ phase, where spectra are dominated by emission lines, as opposed to scattering lines over a quasi-blackbody continuum. The nebular phase is initially in a ‘steady-state’ regime, until thermal reprocessing timescales become long, at which point the temperature and ionization states need to be evolved time-dependently. Since nebular phase spectra offer a possibility of element identification in KN, it is interesting to study the onset and significance of time-dependent effects. I will present a study into these effects conducted using the spectral synthesis code SUMO, and demonstrate that time-dependent calculations may be necessary for certain ejecta parameters. I will also briefly present some ongoing work on the importance of NLTE calculations for post-peak KN, with a focus on consequences for expansion opacities. Hope to see you there! Ana Sagués Carracedo & Davide Gizzi -------------- next part -------------- An HTML attachment was scrubbed... URL: From peter at astro.su.se Wed Feb 23 10:05:53 2022 From: peter at astro.su.se (Peter Lundqvist) Date: Wed, 23 Feb 2022 09:05:53 +0000 Subject: [Okc-wp4] Birthday of SN 1987A.. In-Reply-To: References: <2d9accb3066d43489d1f1566d191f015@astro.su.se> Message-ID: <56436D98-F502-4C66-8DB3-3B71B4B7D93A@astro.su.se> Dear all, I just want to draw to your attention the 35 year anniversary of Supernova 1987A. https://en.wikipedia.org/wiki/SN_1987A#Discovery Searching for ”1987A” in the title on ADS generates 2714 hits… There are certainly more papers than that of this object. Those around in 1987A may refresh their minds: https://ui.adsabs.harvard.edu/abs/1987IAUC.4316....1K/abstract -Peter From davide.gizzi at astro.su.se Thu Feb 24 07:48:59 2022 From: davide.gizzi at astro.su.se (Davide Gizzi) Date: Thu, 24 Feb 2022 06:48:59 +0000 Subject: [Okc-wp4] EO meeting: 3rd of March Message-ID: <68c3bb652a86453aa8e93179c2254383@astro.su.se> Dear all, our next EO meeting will be next Thursday, 3rd of March, at 13:15 (CET). The speaker is Steve Schulze, postdoctoral researcher at the department of Physics, Stockholm University. You can find title and abstract of talk below. To join the meeting: https://stockholmuniversity.zoom.us/j/65883589027?pwd=RGxJOUVQWmNtMlZFMUIwaHRabkExdz09 Meeting ID: 658 8358 9027 Title: The discovery of a new type of core-collapse supernovae and their connection with Wolf-Rayet stars Abstract: The Zwicky Transient Facility (ZTF) monitors the entire northern hemisphere every two nights, pushing the transient discovery rate to a new order of scale. In addition, one of the ZTF partnership surveys scans a smaller area of the sky six times every night. This opens the opportunity to map out existing gaps in the transient phase-space and search for theoretically predicted but not yet detected phenomena. One of those previously unknown transient classes is SN Icn. In 2019, ZTF detected the first member of this new SN class. Recently, Gal-Yam et al. (2022) published the first study on the first SN Icn 2019hgp, followed by Perley et al. (2022), who studied the second SN Icn 2021csp in unprecedented detail. In this talk, I present our current understanding of SNe Icn, how these extreme objects fit in the zoo of other core-collapse SNe, and the implications for our understanding of the fates of massive stars. Hope to see you there! Ana Sagués Carracedo & Davide Gizzi -------------- next part -------------- An HTML attachment was scrubbed... URL: From davide.gizzi at astro.su.se Thu Mar 3 07:59:20 2022 From: davide.gizzi at astro.su.se (Davide Gizzi) Date: Thu, 3 Mar 2022 06:59:20 +0000 Subject: [Okc-wp4] EO meeting: 3rd of March In-Reply-To: <68c3bb652a86453aa8e93179c2254383@astro.su.se> References: <68c3bb652a86453aa8e93179c2254383@astro.su.se> Message-ID: Dear all, a kind reminder of today's EO meeting at 13:15 (CET). Kind regards ________________________________ From: Davide Gizzi Sent: Thursday, February 24, 2022 7:48:59 AM To: Okc-wp4 at fysik.su.se; people at nordita.org Cc: Steve Schulze Subject: EO meeting: 3rd of March Dear all, our next EO meeting will be next Thursday, 3rd of March, at 13:15 (CET). The speaker is Steve Schulze, postdoctoral researcher at the department of Physics, Stockholm University. You can find title and abstract of talk below. To join the meeting: https://stockholmuniversity.zoom.us/j/65883589027?pwd=RGxJOUVQWmNtMlZFMUIwaHRabkExdz09 Meeting ID: 658 8358 9027 Title: The discovery of a new type of core-collapse supernovae and their connection with Wolf-Rayet stars Abstract: The Zwicky Transient Facility (ZTF) monitors the entire northern hemisphere every two nights, pushing the transient discovery rate to a new order of scale. In addition, one of the ZTF partnership surveys scans a smaller area of the sky six times every night. This opens the opportunity to map out existing gaps in the transient phase-space and search for theoretically predicted but not yet detected phenomena. One of those previously unknown transient classes is SN Icn. In 2019, ZTF detected the first member of this new SN class. Recently, Gal-Yam et al. (2022) published the first study on the first SN Icn 2019hgp, followed by Perley et al. (2022), who studied the second SN Icn 2021csp in unprecedented detail. In this talk, I present our current understanding of SNe Icn, how these extreme objects fit in the zoo of other core-collapse SNe, and the implications for our understanding of the fates of massive stars. Hope to see you there! Ana Sagués Carracedo & Davide Gizzi -------------- next part -------------- An HTML attachment was scrubbed... URL: From davide.gizzi at astro.su.se Thu Mar 3 14:49:08 2022 From: davide.gizzi at astro.su.se (Davide Gizzi) Date: Thu, 3 Mar 2022 13:49:08 +0000 Subject: [Okc-wp4] EO meeting: 10th of March Message-ID: Dear all, our next Extreme Object meeting will be next Thursday, 10th of March, at 13:15 (CET). The speaker is Vidushi Sharma, postdoc fellow with Prof. Felix Ryde. See below for title and abstract of the talk. To join the meeting: https://stockholmuniversity.zoom.us/j/65883589027?pwd=RGxJOUVQWmNtMlZFMUIwaHRabkExdz09 Meeting ID: 658 8358 9027 Title: Studying the viewing geometry of sGRBs and central engine using prompt emission Abstract: Prompt emission of short gamma-ray bursts (sGRBs) are analyzed using the model of the multi-color blackbody, which is interpreted as the emission from a non-dissipative photosphere with jet structure and viewing geometry inference. Nearly 69 % and 26 % of the sample is consistent with a multicolor blackbody and a pure blackbody model, respectively. Using this physical interpretation, a narrow jet core with a median of ~ 3 degrees and power-law index of 1.3 - 2.2 as decreasing Lorentz factor profile for the jet structure is deduced. Interestingly, based on the current LIGO sensitivity, the study predicts the rate of coincident detections of bright short GRBs with gravitational waves to be 0.19 - 2.87 events/yr. Another major quest in the field of GRB science is the nature of stellar remnants. Using the magnetar energy limit, 8 GRBs with black hole central engines are identified in 11 years of Fermi GRB sample (long and short both). The estimated masses of these bursts are found to range between 2 - 60 solar masses. A few of them are found to lie in the mass-gap region, suggesting that some of the lighter black holes in the Universe are formed via these catastrophic events. Hope to see you there! Ana Sagués Carracedo & Davide Gizzi -------------- next part -------------- An HTML attachment was scrubbed... URL: From davide.gizzi at astro.su.se Thu Mar 10 08:45:56 2022 From: davide.gizzi at astro.su.se (Davide Gizzi) Date: Thu, 10 Mar 2022 07:45:56 +0000 Subject: [Okc-wp4] EO meeting: 10th of March In-Reply-To: References: Message-ID: Dear all, a reminder of today's EO meeting at 13:15 (CET). Kind regards ________________________________ From: Davide Gizzi Sent: Thursday, March 3, 2022 2:49:08 PM To: Okc-wp4 at fysik.su.se; people at nordita.org Cc: vidushi at kth.se Subject: EO meeting: 10th of March Dear all, our next Extreme Object meeting will be next Thursday, 10th of March, at 13:15 (CET). The speaker is Vidushi Sharma, postdoc fellow with Prof. Felix Ryde. See below for title and abstract of the talk. To join the meeting: https://stockholmuniversity.zoom.us/j/65883589027?pwd=RGxJOUVQWmNtMlZFMUIwaHRabkExdz09 Meeting ID: 658 8358 9027 Title: Studying the viewing geometry of sGRBs and central engine using prompt emission Abstract: Prompt emission of short gamma-ray bursts (sGRBs) are analyzed using the model of the multi-color blackbody, which is interpreted as the emission from a non-dissipative photosphere with jet structure and viewing geometry inference. Nearly 69 % and 26 % of the sample is consistent with a multicolor blackbody and a pure blackbody model, respectively. Using this physical interpretation, a narrow jet core with a median of ~ 3 degrees and power-law index of 1.3 - 2.2 as decreasing Lorentz factor profile for the jet structure is deduced. Interestingly, based on the current LIGO sensitivity, the study predicts the rate of coincident detections of bright short GRBs with gravitational waves to be 0.19 - 2.87 events/yr. Another major quest in the field of GRB science is the nature of stellar remnants. Using the magnetar energy limit, 8 GRBs with black hole central engines are identified in 11 years of Fermi GRB sample (long and short both). The estimated masses of these bursts are found to range between 2 - 60 solar masses. A few of them are found to lie in the mass-gap region, suggesting that some of the lighter black holes in the Universe are formed via these catastrophic events. Hope to see you there! Ana Sagués Carracedo & Davide Gizzi -------------- next part -------------- An HTML attachment was scrubbed... URL: From davide.gizzi at astro.su.se Thu Mar 17 08:21:27 2022 From: davide.gizzi at astro.su.se (Davide Gizzi) Date: Thu, 17 Mar 2022 07:21:27 +0000 Subject: [Okc-wp4] EO meeting: 24th of March Message-ID: Dear all, our next Extreme Object meeting will be next Thursday, 24th of March, at 13:15 (CET). The speaker is Mózsi Kiss from KTH, talking about the XL-Calibur balloon-borne polarimeter. See below for title and abstract of the talk. To join the meeting: https://stockholmuniversity.zoom.us/j/65883589027?pwd=RGxJOUVQWmNtMlZFMUIwaHRabkExdz09 Meeting ID: 658 8358 9027 Title: "T - 7 weeks for the XL-Calibur balloon-borne hard X-ray polarimeter" Abstract: "XL-Calibur is a balloon-borne polarimeter for hard X-rays in the range ~10-80 keV. It is currently scheduled to be launched on a stratospheric balloon from the Esrange Space Center in northern Sweden, for a week-long flight to Canada. The system features an X-ray mirror with a 12 m focal length and a Compton polarimeter with a beryllium scattering element surrounded by pixelated CZT detectors. The giant truss is pointed and stabilized using the Wallops Arc-Second Pointer (WASP), allowing astronomical sources to be acquired and tracked. The main observational targets are the Crab system (pulsar, nebula) and Cygnus X-1, and observations will provide new insights into the emission mechanisms of these sources. Joint observations are planned with other missions such as the recently launched IXPE, AstroSat and NICER. KTH is responsible for the anticoincidence shield surrounding the polarimeter. In this talk, I will present the scientific instrument and our frantic preparations that will hopefully culminate in a launch in mid-May. I will also describe our two main sources and what we hope to learn about them through these observations." Hope to see you there! Ana Sagués Carracedo & Davide Gizzi -------------- next part -------------- An HTML attachment was scrubbed... URL: From stephan.rosswog at astro.su.se Tue Mar 22 21:38:17 2022 From: stephan.rosswog at astro.su.se (Stephan Rosswog) Date: Tue, 22 Mar 2022 20:38:17 +0000 Subject: [Okc-wp4] Fwd: [Int_subscribers] REMINDER: INT 20R-1b - "The r-process and the nuclear EOS after aLIGO's third observing run" References: Message-ID: <2E75500A-089C-4656-8A56-2B0261278E57@astro.su.se> Begin forwarded message: From: INT news list > Subject: [Int_subscribers] REMINDER: INT 20R-1b - "The r-process and the nuclear EOS after aLIGO's third observing run" Date: 22 March 2022 at 20:24:26 CET To: > Reply-To: > Dear Colleague, This is a reminder that the workshop “The r-process and the nuclear EOS after aLIGO's third observing run” (INT 20R-1b) will be held as a hybrid event consisting of both virtual participants and in-person participants visiting the national Institute for Nuclear Theory (INT) at the University of Washington in Seattle, Washington, from May 23 - 27, 2022. Please see the email below. Details of the workshop can be found at: https://sites.google.com/uw.edu/int/programs/20r-1b The organizers of the workshop encourage you to apply by April 1, 2022 for full consideration. The online application link can be found on the webpage. In the comment box of the application form, please write [In-person], [Virtual], or [Either] to reflect your preferred mode of attendance. Please note: All in-person visitors are required to show proof of vaccination against COVID-19 upon arrival to the INT. Please let us know if you have any questions. Best regards, The Organizers: David Radice Jocelyn Read Luke Roberts -- Alesha Vertrees Program Coordinator Institute for Nuclear Theory University of Washington Box 351550 Seattle, WA 98195-1550 From: Int_subscribers > On Behalf Of INT news list Sent: Tuesday, February 22, 2022 2:43 PM To: int_subscribers at u.washington.edu Subject: [Int_subscribers] INT 20R-1b Announcement - "The r-process and the nuclear EOS after aLIGO's third observing run" Dear colleagues, We are organizing the hybrid workshop “The r-process and the nuclear EOS after aLIGO's third observing run” (INT 20R-1b), to be held at the national Institute for Nuclear Theory (INT) at the University of Washington in Seattle, WA, from May 23-27, 2022. We would like to encourage you to apply for admission. We strongly encourage the participation of scientists from underrepresented groups, including women and underrepresented minorities. This event was originally scheduled for March 2020, and we ran an abbreviated online program in April 2020 [1]. The scientific goal of the 2022 workshop is to bring together experts in galactic chemical evolution, numerical relativity, nuclear physics, and both gravitational wave and electromagnetic astronomy to understand the contribution of merger events to r-process nucleosynthesis. We aim to lay the foundations needed to interpret upcoming results from the next LIGO/Virgo/KAGRA observation run, which is currently expected to begin before the end of 2022. The workshop aims to bring together senior and junior researchers in an environment stimulating for discussion and collaboration. This is a "hybrid" workshop, meaning there will be a combination of virtual and in-person participants. We anticipate the schedule will include a selection of talks and open time for discussion and break-outs. More details can be found on the workshop website: https://sites.google.com/uw.edu/int/programs/20r-1b Here you will also find a link to the application form, which we encourage you to submit as soon as possible. We will do our best to accommodate as many of the respondents as we can. For full consideration, please apply by April 1, 2022. The INT generally provides support to defray the cost of in-person workshop participants’ local housing and meal expenses. We hope to see you in Seattle, online or in person. Best regards, David Radice Jocelyn Read Luke Roberts [1] Previous program: https://www.int.washington.edu/PROGRAMS/20-1b/ Institute for Nuclear Theory University of Washington Box 351550 Seattle, WA 98195-1550 Email: intmail at uw.edu Phone: 206-685-3360 [cid:image001.png at 01D83DDC.543D90D0] _______________________________________________ Int_subscribers mailing list Int_subscribers at u.washington.edu http://mailman12.u.washington.edu/mailman/listinfo/int_subscribers ---------------------------------------------- Prof. Dr. Stephan Rosswog Computational High-Energy Astrophysics The Oskar Klein Centre for Cosmoparticle Physics Department of Astronomy, Stockholm University AlbaNova, Roslagstullbacken 21 SE-10691 Stockholm, Sweden Email: stephan.rosswog at astro.su.se Tel.: +46 (0)8 5537 8529 URL: http://compact-merger.astro.su.se/ -------------- next part -------------- An HTML attachment was scrubbed... URL: -------------- next part -------------- A non-text attachment was scrubbed... Name: image001.png Type: image/png Size: 4570 bytes Desc: image001.png URL: From davide.gizzi at astro.su.se Thu Mar 24 07:13:52 2022 From: davide.gizzi at astro.su.se (Davide Gizzi) Date: Thu, 24 Mar 2022 06:13:52 +0000 Subject: [Okc-wp4] EO meeting: 24th of March In-Reply-To: References: Message-ID: <7289fcd20fce4da8b3364ae50e921ad4@astro.su.se> Dear all, a kind reminder of today's EO meeting at 13:15 (CET). Best regards ________________________________ From: Davide Gizzi Sent: Thursday, March 17, 2022 8:21:27 AM To: Okc-wp4 at fysik.su.se; people at nordita.org Cc: Mózsi Kiss Subject: EO meeting: 24th of March Dear all, our next Extreme Object meeting will be next Thursday, 24th of March, at 13:15 (CET). The speaker is Mózsi Kiss from KTH, talking about the XL-Calibur balloon-borne polarimeter. See below for title and abstract of the talk. To join the meeting: https://stockholmuniversity.zoom.us/j/65883589027?pwd=RGxJOUVQWmNtMlZFMUIwaHRabkExdz09 Meeting ID: 658 8358 9027 Title: "T - 7 weeks for the XL-Calibur balloon-borne hard X-ray polarimeter" Abstract: "XL-Calibur is a balloon-borne polarimeter for hard X-rays in the range ~10-80 keV. It is currently scheduled to be launched on a stratospheric balloon from the Esrange Space Center in northern Sweden, for a week-long flight to Canada. The system features an X-ray mirror with a 12 m focal length and a Compton polarimeter with a beryllium scattering element surrounded by pixelated CZT detectors. The giant truss is pointed and stabilized using the Wallops Arc-Second Pointer (WASP), allowing astronomical sources to be acquired and tracked. The main observational targets are the Crab system (pulsar, nebula) and Cygnus X-1, and observations will provide new insights into the emission mechanisms of these sources. Joint observations are planned with other missions such as the recently launched IXPE, AstroSat and NICER. KTH is responsible for the anticoincidence shield surrounding the polarimeter. In this talk, I will present the scientific instrument and our frantic preparations that will hopefully culminate in a launch in mid-May. I will also describe our two main sources and what we hope to learn about them through these observations." Hope to see you there! Ana Sagués Carracedo & Davide Gizzi -------------- next part -------------- An HTML attachment was scrubbed... URL: From davide.gizzi at astro.su.se Thu Mar 31 13:27:49 2022 From: davide.gizzi at astro.su.se (Davide Gizzi) Date: Thu, 31 Mar 2022 11:27:49 +0000 Subject: [Okc-wp4] EO meeting: 7th of April Message-ID: Dear all, our next Extreme Object meeting will be next Thursday, 7th of April, at 13:15 (CET). The speaker is Timothy Linden from Stockholm University. He will talk about how neutron stars can be used to answer questions in fundamental physics. To join the meeting: https://stockholmuniversity.zoom.us/j/65883589027?pwd=RGxJOUVQWmNtMlZFMUIwaHRabkExdz09 Meeting ID: 658 8358 9027 Title: Using Neutron Stars to Probe Fundamental Physics Abstract: Over the past few decades, terrestrial experiments have placed increasingly strong limits on the dark matter-nucleon scattering cross-section. However, a significant portion of the standard dark matter parameter space remains beyond our reach. Due to their extreme density and huge gravitational fields, neutron stars stand as optimal targets to probe dark matter-nucleon interactions. For example, over the last few years, the mere existence of Gyr-age neutron stars has placed strong limits on models of asymmetric dark matter. In this talk, I will discuss novel methods that utilize neutron stars to potentially detect dark matter interactions by studying the galactic morphology of neutron stars, as well as the electromagnetic signals that may be produced via neutron star collapse. Intriguingly, these observations can probe extremely generic dark matter models spanning from MeV - PeV energies, including troublesome portions of parameter space such as pure-Higgsino dark matter. Please note that we are planning to organize the next EO meetings in hybrid format. More information will be provided later on. Kind regards Ana Sagués Carracedo & Davide Gizzi -------------- next part -------------- An HTML attachment was scrubbed... URL: From davide.gizzi at astro.su.se Thu Apr 7 08:15:49 2022 From: davide.gizzi at astro.su.se (Davide Gizzi) Date: Thu, 7 Apr 2022 06:15:49 +0000 Subject: [Okc-wp4] EO meeting: 7th of April In-Reply-To: References: Message-ID: <2c5a8899be224bb88fe878c5ce00a971@astro.su.se> Dear all, a reminder of today's EO meeting at 13:15(CET). Kind regards ________________________________ From: Davide Gizzi Sent: Thursday, March 31, 2022 1:27:49 PM To: Okc-wp4 at fysik.su.se; people at nordita.org Cc: Timothy Linden Subject: EO meeting: 7th of April Dear all, our next Extreme Object meeting will be next Thursday, 7th of April, at 13:15 (CET). The speaker is Timothy Linden from Stockholm University. He will talk about how neutron stars can be used to answer questions in fundamental physics. To join the meeting: https://stockholmuniversity.zoom.us/j/65883589027?pwd=RGxJOUVQWmNtMlZFMUIwaHRabkExdz09 Meeting ID: 658 8358 9027 Title: Using Neutron Stars to Probe Fundamental Physics Abstract: Over the past few decades, terrestrial experiments have placed increasingly strong limits on the dark matter-nucleon scattering cross-section. However, a significant portion of the standard dark matter parameter space remains beyond our reach. Due to their extreme density and huge gravitational fields, neutron stars stand as optimal targets to probe dark matter-nucleon interactions. For example, over the last few years, the mere existence of Gyr-age neutron stars has placed strong limits on models of asymmetric dark matter. In this talk, I will discuss novel methods that utilize neutron stars to potentially detect dark matter interactions by studying the galactic morphology of neutron stars, as well as the electromagnetic signals that may be produced via neutron star collapse. Intriguingly, these observations can probe extremely generic dark matter models spanning from MeV - PeV energies, including troublesome portions of parameter space such as pure-Higgsino dark matter. Please note that we are planning to organize the next EO meetings in hybrid format. More information will be provided later on. Kind regards Ana Sagués Carracedo & Davide Gizzi -------------- next part -------------- An HTML attachment was scrubbed... URL: From ana.sagues-carracedo at fysik.su.se Thu Apr 14 17:22:14 2022 From: ana.sagues-carracedo at fysik.su.se (=?utf-8?B?QW5hIFNhZ3XDqXMgQ2FycmFjZWRv?=) Date: Thu, 14 Apr 2022 15:22:14 +0000 Subject: [Okc-wp4] EO meeting: 21st of April Message-ID: <9E37BE38-D749-4A55-BB6F-19268476B4F5@fysik.su.se> Dear all, our next Extreme Object meeting will be next Thursday, 21st of April, at 13:15 (CET). The speaker is Tuomas Kangas from KTH. He will talk about his recently submitted paper on hydrogen-rich superluminous supernovae. The meeting will be held in hybrid mode at the Albano 3:6228 - Mega room. To join remotely via zoom: https://stockholmuniversity.zoom.us/j/65883589027?pwd=RGxJOUVQWmNtMlZFMUIwaHRabkExdz09 Meeting ID: 658 8358 9027 Title: Power sources of hydrogen-rich superluminous supernovae Abstract: Superluminous supernovae (SLSNe), with their often-extreme luminosity compared with the typical core-collapse supernovae (CCSNe) of massive stars, cannot be explained with the power sources typical to their lower-luminosity counterparts. Analogously to CCSNe, SLSNe are divided into hydrogen-poor (type I) and hydrogen-rich (type II). Most hydrogen-rich SLSNe are clearly powered by interaction with a dense circumstellar medium (CSM) and have spectra with strong narrow emission lines, while hydrogen-poor ones are thought to be powered by the spin-down of a magnetar born in the explosion. In rare cases, SLSNe II with broad emission lines but no narrow lines are found; the power sources of such SNe have been ambiguous, with both magnetars and CSM interaction as possible explanations, but only a few are known in the literature. I present a study based on 14 SLSNe II without narrow lines, the largest such sample to date, discovered and/or followed up by the Zwicky Transient Facility between 2018 and 2020. We have examined the light curves, spectra and host galaxies of these SLSNe and fitted light curve models to them. While light curve models have trouble distinguishing between magnetars and CSM, other signs point toward interaction being the dominant powering mechanism of SLSNe II. The most luminous ones, however, may need another power source as well. Kind regards, Note: We welcome our new organiser Haakon Andresen Ana Sagués Carracedo & Davide Gizzi & Haakon Andresen -------------- next part -------------- An HTML attachment was scrubbed... URL: From ana.sagues-carracedo at fysik.su.se Fri Apr 29 12:05:11 2022 From: ana.sagues-carracedo at fysik.su.se (=?utf-8?B?QW5hIFNhZ3XDqXMgQ2FycmFjZWRv?=) Date: Fri, 29 Apr 2022 10:05:11 +0000 Subject: [Okc-wp4] EO meeting: 5th of May Message-ID: Dear all, our next Extreme Object meeting will be next Thursday, 5th of April, at 13:15 (CET). The speaker is Cecilie Cold a PhD student from DARK (Copenhagen). She will be around from the 4th to the 6th of May and she will present to us some of her research related to type IIn supernovae. She prepared for a talk of 25-30 minutes, so we will have plenty of time for questions. Saying so if anyone wants to share anything with the group let me know, as we might have time for it during the meeting. The meeting will be held in hybrid mode at the Albano 3:6228 - Mega room. Some directions for those that have never been in the Mega room, it is located in Nordita (floor 6 house 3), if you enter from the door on the right of the elevator it is just there. I will be a little in advance to set up the room, and I can open the door for people with no access. To join the meeting: https://stockholmuniversity.zoom.us/j/65883589027?pwd=RGxJOUVQWmNtMlZFMUIwaHRabkExdz09 Meeting ID: 658 8358 9027 Title: The rate of SNe IIn Abstract: Join me in exploring the extreme world of the interacting IIn supernovae! I will present and discuss a new angle on the rate of type IIn supernovae and the possible host galaxy mass bias on the IIn to core-collapse ratio. With the upcoming LSST we will see IIn becoming more important to other areas of astrophysics such as cosmology, because it is expected that most of the gravitationally lensed supernovae from LSST will be IIn. I will also touch upon the similarities and differences between super-luminous IIn and regular type IIn and also the connection between brightness, host galaxy mass and the two classifications. Kind regards, Ana Sagués Carracedo & Haakon Andresen -------------- next part -------------- An HTML attachment was scrubbed... URL: From haakon.andresen at astro.su.se Mon May 16 10:14:05 2022 From: haakon.andresen at astro.su.se (Haakon Andresen) Date: Mon, 16 May 2022 08:14:05 +0000 Subject: [Okc-wp4] EO meeting on the 19th of May Message-ID: Dear everyone, During the next EO meeting, on the 19th of May, we would like to ask everyone to give a short summary of their current work. I have created a google presentation, please add one slide to this document. https://docs.google.com/presentation/d/1X5f02C1jE0arIjfspHP3nTxRqu-_7g3KPz1OxIY_CoU/edit?usp=sharing We will go around the room following the order of the slides and I will moderate the session. Best regards, Haakon Andresen and Ana Sagués Carracedo -------------- next part -------------- An HTML attachment was scrubbed... URL: From haakon.andresen at astro.su.se Wed May 18 10:56:05 2022 From: haakon.andresen at astro.su.se (Haakon Andresen) Date: Wed, 18 May 2022 08:56:05 +0000 Subject: [Okc-wp4] Slides for the EO meeting on May 19th Message-ID: <87a27f6fdf144bc7b5344f7b88ff9fca@astro.su.se> Dear everyone, Please remember to make one slide with a short summary of your current research. Our goal is to give everyone an overview of who is where and who is doing what. It might, therefore, be useful to include which department/group you belong to in your slides/presentation. Link to google slides: https://docs.google.com/presentation/d/1X5f02C1jE0arIjfspHP3nTxRqu-_7g3KPz1OxIY_CoU/edit?usp=sharing Best, Haakon -------------- next part -------------- An HTML attachment was scrubbed... URL: From ana.sagues-carracedo at fysik.su.se Thu Jun 9 13:36:41 2022 From: ana.sagues-carracedo at fysik.su.se (=?utf-8?B?QW5hIFNhZ3XDqXMgQ2FycmFjZWRv?=) Date: Thu, 9 Jun 2022 11:36:41 +0000 Subject: [Okc-wp4] EO meeting: 16th of June Message-ID: <9FDB9ED7-EFB3-47E9-BF45-101F36787057@fysik.su.se> Dear all, our next and last Extreme Object meeting before the summer break will be held next Thursday, 16th of April, at 13:15 (CET). The speaker is Wynn Jacobson-Galan a fellow researcher from Berkeley visiting us in Stockholm next week. The meeting will be held in hybrid mode at the Albano 3:6228 - Mega room. Some directions for those that have never been in the Mega room, it is located in Nordita (floor 6 house 3), if you enter from the door on the right of the elevator it is just there. I will be a little in advance to set up the room, and I can open the door for people with no access. To join the meeting online: https://stockholmuniversity.zoom.us/j/65883589027?pwd=RGxJOUVQWmNtMlZFMUIwaHRabkExdz09 Meeting ID: 658 8358 9027 Title: Watching a Star Explode with the Young Supernova Experiment Abstract: We present multi-wavelength observations of supernova (SN) 2020tlf, the first normal type II-P/L SN with confirmed precursor emission, as detected by the Young Supernova Experiment (YSE) transient survey. The detected pre-explosion emission for ~130 days prior to SN is consistent with either a super-Eddington progenitor wind or a wave-driven eruption. Soon after discovery, “flash” spectroscopy of SN 2020tlf revealed prominent narrow emission lines from shock-ionized circumstellar material (CSM) shed in progenitor mass-loss episodes in the final months before explosion. Following classification, SN 2020tlf was observed in a thorough multi-wavelength follow-up campaign in UV/optical/IR, radio and X-ray bands out to a +300 days after explosion. The nebular phase spectra of SN 2020tlf constrain the possible mass of the red supergiant progenitor to 10-12 Msun. Finally, we present radiative transfer modeling of the SN light curve and spectral evolution, which reveals that the progenitor star had an extended envelope, detached CSM and a heightened mass loss rate. We will discuss how the progenitor and CSM properties of SN 2020tlf fits within the phase space of the small but growing number of SNe with “flash” spectroscopy and pre-explosion eruptions. Furthermore, we will discuss the physical processes capable of producing such luminous precursor emission in a red supergiant in the final year(s) before explosion. Kind regards, Ana Sagués Carracedo & Haakon Andresen -------------- next part -------------- An HTML attachment was scrubbed... URL: From ana.sagues-carracedo at fysik.su.se Mon Jun 20 21:30:02 2022 From: ana.sagues-carracedo at fysik.su.se (=?utf-8?B?QW5hIFNhZ3XDqXMgQ2FycmFjZWRv?=) Date: Mon, 20 Jun 2022 19:30:02 +0000 Subject: [Okc-wp4] EO meeting: 16th of June In-Reply-To: <9FDB9ED7-EFB3-47E9-BF45-101F36787057@fysik.su.se> References: <9FDB9ED7-EFB3-47E9-BF45-101F36787057@fysik.su.se> Message-ID: <20E6A82D-24D8-4C80-B6EA-335EC2FAC385@fysik.su.se> Here the link to the recording of the meeting: https://stockholmuniversity.box.com/s/3mzdkzc0ww6et2h4ific7ori6cg433ns Thank you so much Wynn for a great talk and discussion. Bests, Ana On 9 Jun 2022, at 13:36, Ana Sagués Carracedo > wrote: Dear all, our next and last Extreme Object meeting before the summer break will be held next Thursday, 16th of April, at 13:15 (CET). The speaker is Wynn Jacobson-Galan a fellow researcher from Berkeley visiting us in Stockholm next week. The meeting will be held in hybrid mode at the Albano 3:6228 - Mega room. Some directions for those that have never been in the Mega room, it is located in Nordita (floor 6 house 3), if you enter from the door on the right of the elevator it is just there. I will be a little in advance to set up the room, and I can open the door for people with no access. To join the meeting online: https://stockholmuniversity.zoom.us/j/65883589027?pwd=RGxJOUVQWmNtMlZFMUIwaHRabkExdz09 Meeting ID: 658 8358 9027 Title: Watching a Star Explode with the Young Supernova Experiment Abstract: We present multi-wavelength observations of supernova (SN) 2020tlf, the first normal type II-P/L SN with confirmed precursor emission, as detected by the Young Supernova Experiment (YSE) transient survey. The detected pre-explosion emission for ~130 days prior to SN is consistent with either a super-Eddington progenitor wind or a wave-driven eruption. Soon after discovery, “flash” spectroscopy of SN 2020tlf revealed prominent narrow emission lines from shock-ionized circumstellar material (CSM) shed in progenitor mass-loss episodes in the final months before explosion. Following classification, SN 2020tlf was observed in a thorough multi-wavelength follow-up campaign in UV/optical/IR, radio and X-ray bands out to a +300 days after explosion. The nebular phase spectra of SN 2020tlf constrain the possible mass of the red supergiant progenitor to 10-12 Msun. Finally, we present radiative transfer modeling of the SN light curve and spectral evolution, which reveals that the progenitor star had an extended envelope, detached CSM and a heightened mass loss rate. We will discuss how the progenitor and CSM properties of SN 2020tlf fits within the phase space of the small but growing number of SNe with “flash” spectroscopy and pre-explosion eruptions. Furthermore, we will discuss the physical processes capable of producing such luminous precursor emission in a red supergiant in the final year(s) before explosion. Kind regards, Ana Sagués Carracedo & Haakon Andresen ------------------------------------------------- okc-wp4 at albanova.se mailing list -------------- next part -------------- An HTML attachment was scrubbed... URL: From haakon.andresen at astro.su.se Fri Sep 9 13:05:25 2022 From: haakon.andresen at astro.su.se (Haakon Andresen) Date: Fri, 9 Sep 2022 11:05:25 +0000 Subject: [Okc-wp4] Startup of EO meetings Message-ID: <5c1b4e103a3b4f77a6058693d2540e9c@astro.su.se> Dear colleagues, I am happy to announce that we reconvene with our Extreme Object (EO) meetings next Thursday the 15th of September at the usual time 13:15 (CEST). Following, we will have biweekly meetings. We are going to continue with an hybrid set up, so you can attend in person at the conference room Albano 3:6228 - Mega or connect via zoom: https://stockholmuniversity.zoom.us/j/62363340520 On the 15th, we will kick off with an informal meeting where each member to give a short overview of their research. The goal is to update each other and introduce new members to the ongoing research of the working group. So please add a slide or 2 to introduce yourself and the research that you do or intend to do here: https://docs.google.com/presentation/d/1xS8uARdqNoBb7ANOFiouCCpXJZy6Dv_tWDB8RdIUWok/edit?usp=sharing Following the start-up meeting, we will have our first regular EO meeting on the 29th of September, where Federico Schianchi will present his work on neutron star mergers. Federico Schianchi will be visiting Evan O'Connor's group during the last week of september. On October 4th we have an extra seminar by Andrew Levan, a visitor in Josefin Larsson's group. Note the unusual time, day and room: Tuesday 4th at 10:00 (CEST) in A5:1003 Looking forward to see you all, Kind regards, Ana Sagués Carracedo & Haakon Andresen -------------- next part -------------- An HTML attachment was scrubbed... URL: From ana.sagues-carracedo at fysik.su.se Mon Sep 26 17:01:44 2022 From: ana.sagues-carracedo at fysik.su.se (=?utf-8?B?QW5hIFNhZ3XDqXMgQ2FycmFjZWRv?=) Date: Mon, 26 Sep 2022 15:01:44 +0000 Subject: [Okc-wp4] EO meeting 29th Sept. UNUSUAL ROOM Message-ID: <95473329-193E-4503-962C-235B6352A4A5@fysik.su.se> Dear colleagues, This is a reminder for our next EO meeting next Thursday 29th of September at 13:15 (CEST). The speaker is Federico Schianchi talking about his work on neutron stars mergers. He is visiting Evan's O'Connor's group during this week. The meeting will be fully in person unless personal request. This time the meeting will take place at the commom area of the astronomy department in Albano Hus 3 Plan 4. Following the title and the abstract: Implementation of first-order multipolar radiation transport in Numerical Relativity code BAM Numerical-relativistic simulations of binary neutron star mergers have a key role in Multimessenger Astronomy, e.g., for modeling gravitational and electromagnetic emissions connected to those events. For an accurate description of electromagnetic counterparts, one needs to know the properties of the matter ejected during and shortly after the merger. Inside this material, heavy elements are synthesized depending on the electron fraction of the outflowing matter. The radioactive decay of these elements produce an observable thermal emission that takes the name of Kilonova. All these phenomena are highly dependent on weak interactions between baryons and neutrinos.My work consists of implementing a code that tracks the propagation of such particles and their interaction with matter. It will be part of our Numerical Relativity code BAM. The aim is to get a more accurate estimate of the ejecta properties, mostly of the electron fraction. Recent studies revealed that neutrino emission/absorption also influences the mass and velocity of the ejected material.The scheme is based on a first-order multipolar (M1) transport equation. It consists of evolving the energy and momentum densities of neutrinos without solving a full and too expensive Boltzmann equation.The advantage of transport formalisms with respect to the Leakage scheme currently implemented in BAM is the possibility to take into account for the neutrinos to be reabsorbed by the fluid in another point of the simulation domain, with transfer of energy, momentum and lepton number. Due to the already high computational cost of binary neutron star merger simulations spectral transport schemes are not affordable. We have then to opt for a grey M1 scheme, i.e, we only evolve energy integrated quantities, loosing information on the neutrinos spectrum.Because of this reason the implementation of a more sophisticated scheme like a Monte Carlo transport would be important for the future. Looking forward to see you all, Kind regards, Ana Sagués Carracedo & Haakon Andresen -------------- next part -------------- An HTML attachment was scrubbed... URL: From haakon.andresen at astro.su.se Fri Sep 30 08:31:57 2022 From: haakon.andresen at astro.su.se (Haakon Andresen) Date: Fri, 30 Sep 2022 06:31:57 +0000 Subject: [Okc-wp4] EO seminar 4th 10AM in A5:1003 Message-ID: Hi, Next week we have an extra EO meeting. Andrew Levan from Radboud University. Note the unusual time and location. Best, Haakon (on behalf of the EO organizers ) Tuesday 4th of October ,10:00 A5:1003 Andrew Levan New signatures of compact object mergers The mergers of compact objects (neutron stars and black holes) have now been securely detected via gravitational wave observations and associated with electromagnetic signals in the form of short-duration gamma-ray bursts and kilonovae. The continued identification of further events in both gravitational waves and electromagnetic light remains a high priority for the field but is also very challenging. I will discuss recent evidence linking a subset of long GRBs to compact object mergers and how these events may both enlarge the sample of well-studied mergers and highlight new and hitherto unidentified channels for their formation. -------------- next part -------------- An HTML attachment was scrubbed... URL: From haakon.andresen at astro.su.se Tue Oct 4 09:25:50 2022 From: haakon.andresen at astro.su.se (Haakon Andresen) Date: Tue, 4 Oct 2022 07:25:50 +0000 Subject: [Okc-wp4] Reminder, extra EO meeting today Message-ID: <88259890158841219ebe33050b1f2c6f@astro.su.se> Soon. Tuesday 4th of October ,10:00 A5:1003 Andrew Levan New signatures of compact object mergers The mergers of compact objects (neutron stars and black holes) have now been securely detected via gravitational wave observations and associated with electromagnetic signals in the form of short-duration gamma-ray bursts and kilonovae. The continued identification of further events in both gravitational waves and electromagnetic light remains a high priority for the field but is also very challenging. I will discuss recent evidence linking a subset of long GRBs to compact object mergers and how these events may both enlarge the sample of well-studied mergers and highlight new and hitherto unidentified channels for their formation. From haakon.andresen at astro.su.se Tue Oct 4 11:46:07 2022 From: haakon.andresen at astro.su.se (Haakon Andresen) Date: Tue, 4 Oct 2022 09:46:07 +0000 Subject: [Okc-wp4] Next few EO meetings, call for speakers, and a calendar Message-ID: Hi everyone, After today's extraordinary meeting, there is a two-week gap before our next planned seminar. On the 27th of October, Nora Valtonen-Mattila will speak about high-energy neutrinos from supernovae. Following that, we have Rodrigo Fernandez scheduled for the 24th of November. We want to find a speaker for the 10th of November and, but not as critical, the 13th of October. Please contact Ana or me if you have a suggestion or want to volunteer. We have made a calendar, which I will do my best to keep up to date. You can subscribe to it by using the link below. Let me know if you run into any issues with it. Best, Haakon (on behalf of the EO-meeting organizers) https://ebox.su.se/owa/calendar/498bfd83fc3b4712b479c4492786e06c at astro.su.se/28a1752f7fdb4d53893b0a7feec2e91410595911308686819501/calendar.ics -------------- next part -------------- An HTML attachment was scrubbed... URL: From ana.sagues-carracedo at fysik.su.se Thu Oct 20 13:01:53 2022 From: ana.sagues-carracedo at fysik.su.se (=?utf-8?B?QW5hIFNhZ3XDqXMgQ2FycmFjZWRv?=) Date: Thu, 20 Oct 2022 11:01:53 +0000 Subject: [Okc-wp4] EO meeting 27th October Message-ID: <0C2028DC-C8D0-4BDB-9874-6517BB077FC7@fysik.su.se> Dear all, our next Extreme Object meeting will be next Thursday, 27th of October, at 13:15 (CEST). The speaker is Nora Valtonen-Mattila a PhD from Uppsala Unversity. She will talk about high energy neutrinos from supernova. The meeting will be held in lecture room FC61 at the Astronomy department on the 6th floor in Albanova building. Looking forward to see most of you there. Title: Observing core-collapse supernovae through neutrinos: from MeV to TeV Abstract: Core-collapse supernovae are one of the most energetic events in the cosmos, releasing a tremendous amount of energy in the form of low-energy O(10 MeV) neutrinos before the shock breakout. Some models have also predicted post-explosion emission of high-energy neutrinos O(>TeV) through particle acceleration processes. In this talk, I will explore how we can use both energy ranges to observe supernovae and, in particular, how we can extend the detection horizon of IceCube by using high-energy neutrinos. Kind regards, Ana Sagués Carracedo & Haakon Andresen -------------- next part -------------- An HTML attachment was scrubbed... URL: From ana.sagues-carracedo at fysik.su.se Mon Nov 7 23:49:29 2022 From: ana.sagues-carracedo at fysik.su.se (=?utf-8?B?QW5hIFNhZ3XDqXMgQ2FycmFjZWRv?=) Date: Mon, 7 Nov 2022 22:49:29 +0000 Subject: [Okc-wp4] EO meeting 10th November Message-ID: Dear all, We are having an Extreme Object meeting this week on Thursday 10th November at 13:15 in the Mega room (6th floor, house 3, where Nordita). Our speaker is Katie Freeze’s PhD student visiting us from Texas. He will stay around until the end of the month and will present some of his work to us. Following tittle and abstract: Dark Matter Annihilation in Stars: A New Lease on Life? What happens to a star when fusion isn't the only relevant power source? We explore how introducing non-nuclear energy, such as energy that could come from dark matter annihilation, affects the evolution of massive stars. In particular, we aim to determine whether stars which produce a significant amount of energy from non-nuclear sources can avoid undergoing pair instability supernovae, and can therefore form black holes in the forbidden mass gap between 50 and 140 Msun. Looking forward to see you in a couple of days, Kind regards, Ana Sagués Carracedo & Haakon Andresen -------------- next part -------------- An HTML attachment was scrubbed... URL: From ana.sagues-carracedo at fysik.su.se Tue Nov 8 10:57:53 2022 From: ana.sagues-carracedo at fysik.su.se (=?utf-8?B?QW5hIFNhZ3XDqXMgQ2FycmFjZWRv?=) Date: Tue, 8 Nov 2022 09:57:53 +0000 Subject: [Okc-wp4] EO meeting 10th November In-Reply-To: References: Message-ID: Hi again, Of course, I forgot to add the speakers name in the announcement, my apologies. He is Joshua Ziegler, PhD student visiting from the university of Texas. Best regards, Ana On 7 Nov 2022, at 23:49, Ana Sagués Carracedo > wrote: Dear all, We are having an Extreme Object meeting this week on Thursday 10th November at 13:15 in the Mega room (6th floor, house 3, where Nordita). Our speaker is Katie Freeze’s PhD student visiting us from Texas. He will stay around until the end of the month and will present some of his work to us. Following tittle and abstract: Dark Matter Annihilation in Stars: A New Lease on Life? What happens to a star when fusion isn't the only relevant power source? We explore how introducing non-nuclear energy, such as energy that could come from dark matter annihilation, affects the evolution of massive stars. In particular, we aim to determine whether stars which produce a significant amount of energy from non-nuclear sources can avoid undergoing pair instability supernovae, and can therefore form black holes in the forbidden mass gap between 50 and 140 Msun. Looking forward to see you in a couple of days, Kind regards, Ana Sagués Carracedo & Haakon Andresen ------------------------------------------------- okc-wp4 at albanova.se mailing list -------------- next part -------------- An HTML attachment was scrubbed... URL: From haakon.andresen at astro.su.se Fri Nov 18 13:02:33 2022 From: haakon.andresen at astro.su.se (Haakon Andresen) Date: Fri, 18 Nov 2022 12:02:33 +0000 Subject: [Okc-wp4] EO meeting on the 24th of November Message-ID: <690946f2a824465b9f854563e37a266e@astro.su.se> Dear everyone, The next EO meeting will take place in the MEGA room on the 24th of November. Looking forward to see you all next week! Kind regards, Ana Sagués Carracedo & Haakon Andresen When: 27th of November, 13:15 Where: MEGA Speaker: Rodrigo Fernandez Title: Mass ejection in non-rotating failed supernovae Abstract: The core-collapse of a slowly-rotating massive star that fails to explode results in the formation of a black hole (BH). Below the pair-instability threshold, a protoneutron star phase always precedes BH formation, with a corresponding reduction in the total gravitational mass due to neutrino emission. The ensuing deviation from hydrostatic equilibrium in the outer layers of the star results in the ejection of a small amount of mass with much lower energies than in successful supernovae. The mass and velocity of the ejecta depend on properties of the core and envelope of the progenitor. I'll discuss an exploration of this mechanism over a wide range of stellar progenitors using spherically-symmetric hydrodynamic simulations, focusing on the effect of the dense-matter equation of state and spatial resolution on the ejecta properties, expected electromagnetic counterparts, and upper limits to the mass of the BH remnant. -------------- next part -------------- An HTML attachment was scrubbed... URL: From haakon.andresen at astro.su.se Fri Nov 18 13:03:58 2022 From: haakon.andresen at astro.su.se (Haakon Andresen) Date: Fri, 18 Nov 2022 12:03:58 +0000 Subject: [Okc-wp4] EO meeting on the 24th of November In-Reply-To: <690946f2a824465b9f854563e37a266e@astro.su.se> References: <690946f2a824465b9f854563e37a266e@astro.su.se> Message-ID: I just notice my typo. It should be When: 24th of November, 13:15. ________________________________ From: Okc-wp4-at-fysik.su.se on behalf of Haakon Andresen Sent: 18 November 2022 13:02:33 To: Okc-wp4 at fysik.su.se Subject: [Okc-wp4] EO meeting on the 24th of November Dear everyone, The next EO meeting will take place in the MEGA room on the 24th of November. Looking forward to see you all next week! Kind regards, Ana Sagués Carracedo & Haakon Andresen When: 27th of November, 13:15 Where: MEGA Speaker: Rodrigo Fernandez Title: Mass ejection in non-rotating failed supernovae Abstract: The core-collapse of a slowly-rotating massive star that fails to explode results in the formation of a black hole (BH). Below the pair-instability threshold, a protoneutron star phase always precedes BH formation, with a corresponding reduction in the total gravitational mass due to neutrino emission. The ensuing deviation from hydrostatic equilibrium in the outer layers of the star results in the ejection of a small amount of mass with much lower energies than in successful supernovae. The mass and velocity of the ejecta depend on properties of the core and envelope of the progenitor. I'll discuss an exploration of this mechanism over a wide range of stellar progenitors using spherically-symmetric hydrodynamic simulations, focusing on the effect of the dense-matter equation of state and spatial resolution on the ejecta properties, expected electromagnetic counterparts, and upper limits to the mass of the BH remnant. -------------- next part -------------- An HTML attachment was scrubbed... URL: From haakon.andresen at astro.su.se Thu Nov 24 12:03:22 2022 From: haakon.andresen at astro.su.se (Haakon Andresen) Date: Thu, 24 Nov 2022 11:03:22 +0000 Subject: [Okc-wp4] EO meeting on the 24th of November In-Reply-To: References: <690946f2a824465b9f854563e37a266e@astro.su.se>, Message-ID: Reminder Speaker: Rodrigo Fernandez Title: Mass ejection in non-rotating failed supernovae ________________________________ From: Okc-wp4-at-fysik.su.se on behalf of Haakon Andresen Sent: 18 November 2022 13:03:58 To: Okc-wp4 at fysik.su.se Subject: Re: [Okc-wp4] EO meeting on the 24th of November I just notice my typo. It should be When: 24th of November, 13:15. ________________________________ From: Okc-wp4-at-fysik.su.se on behalf of Haakon Andresen Sent: 18 November 2022 13:02:33 To: Okc-wp4 at fysik.su.se Subject: [Okc-wp4] EO meeting on the 24th of November Dear everyone, The next EO meeting will take place in the MEGA room on the 24th of November. Looking forward to see you all next week! Kind regards, Ana Sagués Carracedo & Haakon Andresen When: 27th of November, 13:15 Where: MEGA Speaker: Rodrigo Fernandez Title: Mass ejection in non-rotating failed supernovae Abstract: The core-collapse of a slowly-rotating massive star that fails to explode results in the formation of a black hole (BH). Below the pair-instability threshold, a protoneutron star phase always precedes BH formation, with a corresponding reduction in the total gravitational mass due to neutrino emission. The ensuing deviation from hydrostatic equilibrium in the outer layers of the star results in the ejection of a small amount of mass with much lower energies than in successful supernovae. The mass and velocity of the ejecta depend on properties of the core and envelope of the progenitor. I'll discuss an exploration of this mechanism over a wide range of stellar progenitors using spherically-symmetric hydrodynamic simulations, focusing on the effect of the dense-matter equation of state and spatial resolution on the ejecta properties, expected electromagnetic counterparts, and upper limits to the mass of the BH remnant. -------------- next part -------------- An HTML attachment was scrubbed... URL: