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<p>A toda la comunidad, <br>
</p>
<p>a continuación les reenviamos información sobre la reunión
SuperVirtual 2023, la cual se llevará a cabo entre los <b>días 6
y 10 de noviembre próximos.</b></p>
<p>Saludos,</p>
<p>Secyt-FCAG<br>
<span
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px"></span></p>
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-------- Mensaje reenviado --------<br>
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<div class="gmail_quote"><span
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px">Dear
colleagues,</span><br
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px">
<div dir="ltr"><br
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px">
<span
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px">We
are delighted to make the first announcement for
SuperVirtual 2023</span><span
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px">.</span><span
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px"><span> </span>The
meeting will be held in virtual mode from November 6th
to 10th, 2023.</span>
<div><br
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px">
<span
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px">As
in SuperVirtual 2022, SuperVirtual 2023 will cover
both core-collapse and thermonuclear supernovae, as
well as some of the novel transients that are being
found by current surveys. While in person conferences
are now thankfully resuming, we hope that this
online-only meeting will continue to provide a useful
addition. In particular we intend for SuperVirtual
2023 to offer an opportunity to attendees who have
travel or financial restrictions. </span><span
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px">SuperVirtual
2023 aims to organise a conference that is as
inclusive and participatory as possible. It is planned
that both the selection of focus topics and that of
contributed speakers will make significant use of
participant input - more details of this will be
circulated at a later date. </span><span
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px">Please
note that the time zone of the conference has been
changed from 2022, and for this year we will start
each day at 14:00 UTC. This is to allow those in
unfavourable time zones last year to connect at a more
comfortable time.</span><br
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px">
<br
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px">
<span
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px">For
more information, please visit the conference website.</span><br
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px">
<span
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px"><a
href="https://sites.google.com/view/supervirtual2023/" target="_blank"
moz-do-not-send="true" class="moz-txt-link-freetext">https://sites.google.com/view/supervirtual2023/</a></span><br
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px">
<br
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px">
<span
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px">Organization
committee</span><br
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px">
<span
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px">Joe
Anderson (European Southern Observatory, Chile)</span><br
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px">
<span
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px">Melina
Cecilia Bersten (National University of La Plata,
Argentina)</span><br
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px">
<span
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px">Janet
Ting-Wan Chen (National Central University, Taiwan)</span><br
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px">
<span
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px">Morgan
Fraser (University College Dublin, Ireland)</span><br
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px">
<span
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px">Kate
Maguire (Trinity College Dublin, Ireland)</span><br
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px">
<span
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px">Raffaella
Margutti (University of California, Berkeley, USA)</span><br
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px">
<span
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px">Takashi
Moriya (National Astronomical Observatory of Japan,
Japan)</span><br
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px">
<span
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px">Ken
Shen (University of California, Berkeley, USA)</span><br
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px">
<br
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px">
<span
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px">Scientific
Rationale</span><br
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px">
<span
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px">Wide-field
transient surveys are currently delivering large
statistical samples of supernovae (SNe), while also
discovering peculiar and exotic events. New and
up-coming facilities will provide another leap in
sample sizes or afford new observations at distinct
wavelengths and out to late epochs. Samples of
‘standard’ supernovae enable strong constraints on
their progenitor properties and explosion mechanisms.
Meanwhile, the discovery of peculiar explosions often
challenges our application of standard SN physics to
such emerging classes. In addition, the early
detection of nearby transients can lead to a plethora
of constraints on progenitors, explosion mechanisms,
and stellar evolution - as exemplified by the recent
case of SN2023ixf. SuperVirtual 2023 will address many
of these developments - providing a review of SN
observations and physics, while exploring the limits
of our current understanding of the processes driving
SN diversity.</span><br
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px">
<span
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px">There
is now strong consensus that the majority of
hydrogen-rich SNeII arise from massive red supergiant
stars. However, there is still disagreement on the
exact mapping from progenitor and explosion properties
to transient characteristics. The last decade has seen
mounting evidence that at least a significant fraction
of stripped-envelope-SNe arise from binary systems,
although which envelope-mass stripping process
dominates for which progenitors is still debated. In
addition, it now appears that ejecta-CSM interaction
is not only important for our understanding of
narrow-line SNeIIn, but may also be critical for many
other SN types - especially at early times in their
evolution. This understanding is being enhanced by
advances in survey and follow up capabilities -
observations of which will be discussed at this
meeting.</span><br
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px">
<span
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px">Knowledge
of the progenitors and explosion mechanisms of SNeIa
continues to grow, with larger statistical samples in
addition to higher quality data of individual
explosions. Such data includes observations within
hrs/days of explosion, affording investigation into
the prevelance of early 'excess emission' that
constrains the progenitor scenario. Very late-time
observations constrain the isotopic abundances
produced in SNeIa, thus constraing the explosion
mechanism. However, it is still unclear which
progenitor systems produce the bulk of the SNIa
population. This conference will provide a platform to
discuss new observations, progenitor and explosion
modelling, and possible future strategies to constrain
the SNIa phenomenon.</span><br
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px">
<span
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px">The
number of ‘non-standard’ SNe also continues to grow.
Samples now exist of exotic explosions such as
superluminous SNe (SLSNe) and SNeIbn. However, in the
former it is still unclear which powering mechanism
enables such large luminosities, while the properties
of the latter challenge our understanding of late-time
stellar evolution. Meanwhile, the diversity and number
of 'peculiar' thermonuclear SNe continues to grow -
from SNIax to .Ia explosions. SuperVirtual 2023 will
motivate discussion on the state of the art of the
explosion physics and progenitor evolution required to
explain these diverse events. There are also a number
of classes where only a few well-observed events
exist. ‘Fast transients’ (coming in different flavours
with different nomenclature - e.g. ‘FBOTs’) have
timescales making them difficult to observe, but
additionally have properties that are difficult to
understand without invoking exotic physical scenarios.
One of the most recent additions to the SN family is
the SNIcn class, which further stretches the family of
SNe that are significantly affected by ejecta-CSM
interaction. Finally, together with these new classes,
a larger number of SNe are discovered with specific
features that also require an extension of any
standard SN model - e.g. short timescale modulations
in light curve shapes.</span><br
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px">
<span
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px">A
full understanding of the SN phenomenon and its
diversity is only possible through comparing transient
observations with predictions from explosion models
and stellar evolution. At SuperVirtual 2023, SN
observations will be confronted with the latest
modelling of stellar explosions to survey the current
landscape of SNe, their numerous different classes,
and their progenitor populations.</span><br
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px">
<span
style="color:rgb(0,0,0);font-family:Helvetica;font-size:14px">SuperVirtual
2023 aims to organise a conference that is as
inclusive and participatory as possible. It is planned
that both the selection of focus topics and that of
contributed speakers will make significant use of
participant input - more details of this will be
circulated at a later date.<span> </span></span><br>
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