ISSN 1783-3426
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Proposed IAU Commission on Stellar
Magnetism
voting for the new
Commission on Massive Stars
UV
astronomy commission proposal
Reminder:
voting for a new IAU Commission
The impact of mass-loss on the
evolution and pre-supernova properties of red supergiants
Luminous
Blue Variables and superluminous supernovae from binary
mergers
Analytical Solutions for
Radiation-Driven Winds in Massive Stars. I: The
Line-Driven
Winds Revisited in the Context of Be Stars: Ω-slow Solutions with
High k Values
The MiMeS Survey of
Magnetism in Massive Stars: CNO surface abundances of Galactic O
stars
New multiwavelength
observations of the Of?p star CPD -28 2561
SXP
5.05 = IGR J00569-7226 : using X-rays to explore the structure of a
Be stars circumstellar disk
Spectroscopic Instrumentation – Fundamentals and Guidelines for Astronomers
Closed (original deadline passed):
Research Fellow - Nuclear
Astrophysics
1 Postdoc and 2 PhD
Positions at the University of Tübingen
Postdoctoral
and PhD positions in the framework of the ESA project "Hubble
Catalogue of Variables"
Open:
Three-year postdoctoral research
position on the formation of massive stars
Lecturer/Senior
Lecturer position in astronomy or astrophysics at Monash
PhD
Studentships (STFC/Keele funding) in Astronomy/Astrophysics
Stellar
Physics in Galaxies throughout the Universe
Massive
Stars and the Gaia-ESO Survey
In the context of the IAU
Commission renewal process, a new Commission on Stellar Magnetism has
been proposed.
To quote from the Letter of Intent:
"Considering the diverse and universal impact of stellar
magnetism on the physics of stars, the clear scientific and societal
importance of major unsolved problems in the field (e.g. the solar
dynamo, space weather), and the large, broad international community
engaged in this field, we propose the organization of a
Commission on Stellar Magnetism with the aim of facilitating
progress in understanding all aspects of stellar magnetism
and activity, and in particular to coordinate international
efforts in this regard. We welcome all individuals interested in
pursuing the goals of the Commission."
Over 50 new
Commissions have been proposed, including 8 in Division G ("Stars
and Stellar Physics").
Members of the IAU should have
recently received an email invitation to vote for up to 3 of the
proposed commissions as part of an "Expression of Interest"
activity.
We invite Massive Stars WG members to review the
proposed Stellar Magnetism Commission LOI.
Weblink:
http://www.iau.org/submissions/commissionproposal/list
Email:
wade-g@rmc.ca
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dear Massive Stars Working
Group members,
the IAU has started the voting procedure for the
new Commissions.
As we announced a few weeks ago, the Organizing
Committee of the
Massive Stars Working Group has submitted a
Letter of Interest to turn our
Working Group into an IAU
Commission, following previous WG decissions.
The OC
encourages all WG members that are also IAU members to vote for the
new Commission on Massive Stars following the instructions given
in the email
sent by the IAU General Secretary (to IAU members).
The OC also encourages all WG members to send comments and
suggestions
on the LoI for the final proposal. Please send them
before December 31 to
me (ahd@iac.es) or any OC member.
with
best regards,
Artemio Herrero,
chair, on behalf of the
Massive Stars Working Group Organizing Committee
Weblink:
Email: ahd@iac.es
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Dear colleagues and
aficionados of ultraviolet astronomy:
Those of you who are
members of the IAU will have received yesterday or today an Email
from the General Secretary Thierry Montmerle announcing the start of
the “indicative voting” for the new Commissions that were
proposed earlier. This, because all existing Commissions will cease
to exist at the coming General Assembly (GA) in August 2015 and the
new ones will be established.
If you browsed through the list
of commissions visible at
http://www.iau.org/submissions/commissionproposal/list/, you probably
noticed NC-19, which is our proposal to establish a Commission to
deal with UV astronomy. The need for this Commission became evident
at the last GA in Beijing, since the parent Division (XI) morphed
into Division D that deals only with high energy astrophysics.
We
believe that a dedicated Commission will play a major role in
promoting the UV domain to a place of prominence among the different
spectral domains, perhaps as much (or more) that the X-ray and IR,
both in securing space missions and in educating a new generation of
UV astronomers.
In order to secure these goals, we urge you
to vote for NC-19 and to convince your colleagues to do the same.
Please spread the word and make sure you finalize your vote before 31
December. If you are NOT a member of the IAU and have not received
the GS Email, you can still help by convincing your colleagues who
ARE members to vote for NC-19.
Thank you for your help, and
hoping to revitalize UV astronomy,
Ana Ines Gomez de Castro,
Jayant Murthy, Noah Brosch (proposers)
Weblink:
Email:
Noah@wise.tau.ac.il
Back to contents
dear MSWG members,
(you may
skip this message if you are not an IAU member or if you already
voted for new Commissions)
as you know, we are in the process
of applying to become a new IAU Commission, the Massive Stars
Commission. In Beijing our group considered that this is an excellent
opportunity for our research area. We think it will also contribute
to the IAU long-term objectives.
Our group has been very
active since its creation. This sustained activity is one of our
strengths. Now we have to keep active and participate in the poll the
IAU has created to explore the interest of the community in the new
commissions.
The intermediate results are not bad for our
proposal (4th out of 8 proposals in Division G), but it is important
to get as many votes as possible.
If you are an IAU member
and still didn't vote, the MSWG-OC encourages you to vote for the new
Massive Stars Commission. The poll is open until December 31th.
with best regards,
Artemio Herrero
chair, on behalf
of the Massive Stars Working Group Organizing Committee
Weblink:
Email: ahd@iac.es
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G. Meynet (1), V. Chomienne (1), S. Ekstrom (1) , C. Georgy
(2), A. Granada (1), J. Groh (1), A. Maeder (1), P. Eggenberger (1),
E. Levesque (3) and P. Massey (4)
(1) Geneva Observatory,
University of Geneva, Maillettes 51, CH-1290 Sauverny, Switzerland
(2) Astrophysics, Lennard-Jones Laboratories, EPSAM, Keele
University, Staffordshire ST5 5BG, UK
(3) CASA, Department of
Astrophysical and Planetary Sciences, University of Colorado 389-UCB,
Boulder, CO 80309, USA
(4) Lowell Observatory, 1400 W Mars
Hill Road, Flagstaff, AZ 86001, USA
The post main-sequence
evolution of massive stars is very sensitive to many parameters of
the stellar models. Key parameters are the mixing processes, the
metallicity, the mass-loss rate and the effect of a close companion.
We study how the red supergiant lifetimes, the tracks in the
Hertzsprung-Russel diagram (HRD), the positions in this diagram of
the pre-supernova progenitor as well as the structure of the stars at
that time change for various mass-loss rates during the red
supergiant phase (RSG), and for two different initial rotation
velocities. Stellar models are computed with the Geneva code for
initial masses between 9 and 25 M$_odot$ at solar metallicity
(Z=0.014) with 10 times and 25 times the standard mass-loss rates
during the red supergiant phase, with and without rotation. The
surface abundances of RSGs are much more sensitive to rotation than
to the mass-loss rates during that phase.
A change of the RSG
mass-loss rate has a strong impact on the RSG lifetimes and therefore
on the luminosity function of RSGs. An observed RSG is associated to
a larger initial mass model, when enhanced RSG mass-loss rate models
are used to deduce that mass. At solar metallicity, the enhanced
mass-loss rate models do produce significant changes on the
populations of blue, yellow and red supergiants. When extended blue
loops or blue ward excursions are produced by enhanced mass-loss, the
models predict that a majority of blue (yellow) supergiants are post
RSG objects. These post RSG stars are predicted to show much smaller
surface rotational velocities than similar blue supergiants on their
first crossing of the HR gap. Enhanced mass-loss rates during the red
supergiant phase has little impact on the Wolf-Rayet (WR)
populations. The position in the HRD of the end point of the
evolution depends on the mass of the hydrogen envelope. More
precisely, whenever, at the pre-supernova stage, the H-rich envelope
contains more than about 5% of the initial mass, the star is a red
supergiant, and whenever the H-rich envelope contains less than 1% of
the total mass the star is a blue supergiant. For intermediate
situations, intermediate colors/effective temperatures are obtained.
Yellow progenitors for core collapse supernovae can be explained by
the enhanced mass-loss rate models, while the red progenitors are
better fitted by the standard mass-loss rate models.
Reference:
in press for Astronomy and Astrophysics
Status: Manuscript has
been accepted
Weblink:
http://arxiv.org/abs/1410.8721
Comments:
Email: georges.meynet@unige.ch
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Stephen Justham (1), Philipp Podsiadlowski (2), Jorick S.
Vink (3)
1 - National Astronomical Observatories, The
Chinese Academy of Sciences, Beijing, China
2 - Astrophysics
Sub-Department, University of Oxford, Oxford OX1 3RH, UK
3 -
Armagh Observatory, College Hill, Armagh, BT619DG, UK
Evidence
suggests that the direct progenitor stars of some core-collapse
supernovae (CCSNe) are luminous blue variables (LBVs), perhaps
including some `superluminous supernovae' (SLSNe). We examine models
in which massive stars gain mass soon after the end of core hydrogen
burning. These are mainly intended to represent mergers following a
brief contact phase during early Case B mass transfer, but may also
represent stars which gain mass in the Hertzsprung Gap or extremely
late during the main-sequence phase for other reasons. The
post-accretion stars spend their core helium-burning phase as blue
supergiants (BSGs), and many examples are consistent with being LBVs
at the time of core collapse. Other examples are yellow supergiants
at explosion. We also investigate whether such post-accretion stars
may explode successfully after core collapse. The final core
properties of post-accretion models are broadly similar to those of
single stars with the same initial mass as the pre-merger primary
star. More surprisingly, when early Case B accretion does affect the
final core properties, the effect appears likely to favour a
successful SN explosion, i.e., to make the core properties more like
those of a lower-mass single star. However, the detailed structures
of these cores sometimes display qualitative differences to any
single-star model we have calculated. The rate of appropriate binary
mergers may match the rate of SNe with immediate LBV progenitors; for
moderately optimistic assumptions we estimate that the progenitor
birthrate is ~1% of the CCSN rate.
Reference: The
Astrophysical Journal (in press); see also arXiv:1410.2426
Status:
Manuscript has been accepted
Weblink:
http://arxiv.org/abs/1410.2426
Comments:
Email: sjustham@nao.cas.cn
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Ignacio Araya(1), Michel Cure(1) and Lydia S.
Cidale(2)
(1) Instituto de Fisica y Astronomia,
Universidad de Valparaıso, Chile;
(2) Departamento de
Espectroscopıa, Facultad de Ciencias Astronomicas y Geofısicas,
Universidad Nacional de La Plata and Instituto de Astrofısica La
Plata, CCT La Plata, CONICET-UNLP,
Accurate mass-loss rate
estimates are crucial keys in the study of wind properties of massive
stars and for testing different evolutionary scenarios. From a
theoretical point of view, this implies solving a complex set of
differential equations in which the radiation field and the
hydrodynamics are strongly coupled. The use of an analytical
expression to represent the radiation force and the solution of the
equation of motion has many advantages over numerical integrations.
Therefore, in this work, we present an analytical expression as a
solution of the equation of motion for radiation-driven winds in
terms of the force multiplier parameters. This analytical expression
is obtained by employing the line acceleration expression given by
Villata and the methodology proposed by Müller & Vink. On the
other hand, we find useful relationships to determine the parameters
for the line acceleration given by Müller & Vink in terms of the
force multiplier parameters.
Reference: ApJ, 795 81
(2014)
Status: Other
Weblink:
http://arxiv.org/abs/1411.0751
Comments:
Email: michel.cure@uv.cl
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Jessie Silaj(1), Michel Cure(2), Carol E. Jones(1)
(1)
Department of Physics and Astronomy, The University of Western
Ontario, Canada
(2) Instituto de Fisica y Astronomıa,
Universidad de Valparaıso, Chile
The standard, or fast,
solutions of m-CAK line-driven wind theory cannot
account for
slowly outflowing disks like the ones that surround Be stars. It
has
been previously shown that there exists another family of solutions
--- the
$Omega$-slow solutions --- that is characterized by much
slower terminal
velocities and higher mass-loss rates. We have
solved the one-dimensional m-CAK
hydrodynamical equation of
rotating radiation-driven winds for this latter
solution,
starting from standard values of the line force parameters ($alpha$,
$k$, and $delta$), and then systematically varying the values of
$alpha$ and
$k$. Terminal velocities and mass-loss rates that are
in good agreement with
those found in Be stars are obtained from
the solutions with lower $alpha$ and
higher $k$ values.
Furthermore, the equatorial densities of such solutions are
comparable to those that are typically assumed in ad hoc models.
For very high
values of $k$, we find that the wind solutions
exhibit a new kind of behavior.
Reference: ApJ 795, 78
(2014)
Status: Other
Weblink:
http://arxiv.org/abs/1411.1465
Comments:
Email: michel.cure@uv.cl
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F. Martins $^1$, A. Hervé $^1$, J.-C. Bouret $^2$, W.
Marcolino $^3$, G.A. Wade $^4$, C. Neiner $^5$, E. Alecian $^6$, J.
Grunhut $^7$, V. Petit $^8$, the MiMeS collaboration
1-
LUPM, CNRS & Montpellier University; 2- LAM Marseille; 3-
Observatorio do Valongo; 4- Royal Military College of Canada; 5-
Observatoire de Paris - LESIA; 6- IPAG Grenoble; 7- ESO; 8-
University of Delaware
The evolution of massive stars is still
partly unconstrained. Mass, metallicity, mass loss and rotation are
the main drivers of stellar evolution. Binarity and magnetic field
may also significantly affect the fate of massive stars. Our goal is
to investigate the evolution of single O stars in the Galaxy. For
that, we use a sample of 74 objects comprising all luminosity classes
and spectral types from O4 to O9.7. We rely on optical spectroscopy
obtained in the context of the MiMeS survey of massive stars. We
perform spectral modelling with the code CMFGEN. We determine the
surface properties of the sample stars, with special emphasis on
abundances of carbon, nitrogen and oxygen. Most of our sample stars
have initial masses in the range 20 to 50 Msun. We show that nitrogen
is more enriched and carbon/oxygen more depleted in supergiants than
in dwarfs, with giants showing intermediate degrees of mixing. CNO
abundances are observed in the range of values predicted by
nucleosynthesis through the CNO cycle. More massive stars, within a
given luminosity class, appear to be more chemically enriched than
lower mass stars. We compare our results with predictions of three
types of evolutionary models and show that, for two sets of models,
80% of our sample can be explained by stellar evolution including
rotation. The effect of magnetism on surface abundances is
unconstrained. Our study indicates that, in the 20-50 Msun mass
range, the surface chemical abundances of most single O stars in the
Galaxy are fairly well accounted for by stellar evolution of rotating
stars.
Reference: Accepted in A&A
Status:
Manuscript has been accepted
Weblink:
http://arxiv.org/abs/1411.4420
Comments:
Email: fabrice.martins@univ-montp2.fr
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S. Hubrig (1), M. Schoeller (2), A. Kholtygin (3), H.
Tsumura (4), A. Hoshino (4), S. Kitamoto (4), L. Oskinova (5), R.
Ignace (6), H. Todt (5), I. Ilyin (1)
(1) AIP, (2) ESO,
(3) St. Petersburg State University, (4) Rikkyo University, (5)
Universitaet Potsdam, (6) East Tennessee State University
A
rather strong mean longitudinal magnetic field of the order of a few
hundred Gauss was detected a few years ago in the Of?p star CPD -28
2561 using FORS2 low-resolution spectropolarimetric observations. In
this work we present additional low-resolution spectropolarimetric
observations obtained during several weeks in 2013 December using
FORS2 (FOcal Reducer low dispersion Spectrograph) mounted at the 8-m
Antu telescope of the VLT. These observations cover a little less
than half of the stellar rotation period of 73.41d mentioned in the
literature. The behaviour of the mean longitudinal magnetic field is
consistent with the assumption of a single-wave variation during the
stellar rotation cycle, indicating a dominant dipolar contribution to
the magnetic field topology. The estimated polar strength of the
surface dipole B_d is larger than 1.15kG. Further, we compared the
behaviour of the line profiles of various elements at different
rotation phases associated with different magnetic field strengths.
The strongest contribution of the emission component is observed at
the phases when the magnetic field shows a negative or positive
extremum. The comparison of the spectral behaviour of CPD -28 2561
with that of another Of?p star, HD148937 of similar spectral type,
reveals remarkable differences in the degree of variability between
both stars. Finally, we present new X-ray observations obtained with
the Suzaku X-ray Observatory. We report that the star is X-ray bright
with log L_X/L_bol ~= -5.7. The low resolution X-ray spectra reveal
the presence of a plasma heated up to 24MK. We associate the 24MK
plasma in CPD -28 2561 with the presence of a kG strong magnetic
field capable to confine stellar wind.
Reference:
MNRAS
Status: Manuscript has been accepted
Weblink:
http://arxiv.org/abs/1412.1658
Comments:
Email: mschoell@eso.org
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M. J. Coe(1), E. S. Bartlett(2), A.J.
Bird(1), F. Haberl(3), J. A. Kennea(4), V.A. McBride(2;5)
L.J.
Townsend(2) & A. Udalski(6)
1 Physics and Astronomy,
University of Southampton, SO17 1BJ, UK.
2 Astronomy, Gravity and
Cosmology Centre, Department of Astronomy, University of Cape Town,
Rondebosch, 7701, South Africa.
3 Max-Planck-Institut f ¨ur
extraterrestrische Physik, Giessenbachstraße, 85748 Garching,
Germany
4 Department of Astronomy and Astrophysics, The
Pennsylvania State University, University Park, PA 16802, USA.
5
South African Astronomical Observatory, PO Box 9, Observatory, 7935,
South Africa.
6 Warsaw University Observatory, Aleje Ujazdowskie
4, 00-478 Warsaw, Poland
On MJD 56590-1 (2013 Oct 25-26)
observations of the Magellanic Clouds by the
INTErnational
Gamma-Ray Astrophysics Laboratory (INTEGRAL) observatory discovered
a previously-unreported bright, flaring X-ray source. This source
was initially
given the identification IGR J00569-7226.
Subsequent multi-wavelength observations
identified the system as
new Be/X-ray binary system in the Small Magellanic Cloud.
Follow-up
X-ray observations by Swift and XMM-Newton revealed an X-ray pulse
period of 5.05s and that the system underwent regular
occulation/eclipse behaviour
every 17d. This is the first
reported eclipsing Be/X-ray binary system in the SMC,
and only
the second such system known to date. Furthermore, the nature of the
occultation
makes it possible to use the neutron star to “X-ray”
the circumstellar disk,
thereby, for the first time, revealing
direct observational evidence for its size and
clumpy structure.
Swift timing measurements allowed for the binary solution to be
calculated from the Doppler shifted X-ray pulsations. This
solution suggests this is
a low eccentricity binary relative to
others measured in the SMC. Finally it is interesting
to note
that the mass determined from this dynamical method for the Be star
( 13 solar masses) is significantly different from that inferred
from the spectroscopic classification
of B0.2Ve ( 16 solar
masses) - an effect that has been noted for some other high
mass
X-ray binary (HMXB) systems.
Reference: MNRAS (in
press)
Status: Manuscript has been accepted
Weblink:
http://arxiv.org/abs/1412.3270
Comments:
Email: mjcoe@soton.ac.uk
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Thomas Eversberg & Klaus
Vollmann
Schnörringen Telescope Science Institute
The
university textbook has 653 pages and contains
- all
spectrograph fundamentals and mathematical basics (standard and
echelle) necessary for instrumental designers, student and scientist,
- fundamental considerations on refractive and reflective
optics
- practical examples (some well-known achievements
from the amateur domain are included),
- periphery
instrumentation (e.g., CCD, fibers, image slicers),
-
theoretical and practical aspects of data reduction and consideration
of errors,
- example massive star physics and
-
prospects in spectropolarimetry.
The book delivers all
necessary tools for a complete and detailed spectrograph design. In
other words, all relevant calculations are performed in detail –
you will not find the frustrating but common phrase “as one can
easily see”.
Reference: Springer Praxis Books -
Astronomy and Planetary Sciences
Status: Other
Weblink:
http://www.springer.com/astronomy/astronomy%2C+observations+and+techniques/book/978-3-662-44534-1
Comments:
Email: thomas.eversberg@dlr.de
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Closed Job Offers (original deadline passed)
Alexander Heger
Monash Centre for Astrophysics
School of Mathematical Sciences
Building 28, M401
Monash
University, VIC 3800
Australia
Applications are invited
for a full time research fellow (Level A/B) in the wider field of
stellar evolution and nuclear astrophysics with Prof. Alexander Heger
at the Monash Centre for Astrophysics (MoCA) at Monash University,
Melbourne, Australia.
The successful candidate must hold, or
be about to obtain, a Ph.D. degree in a relevant discipline and
should have experience in theoretical or numerical modelling in
nuclear astrophysics in one or several of the following fields:
formation and evolution of massive or very massive stars, supernovae,
binary stars, stellar rotation and magnetic fields, gamma-ray burst
and other transients and outbursts, galactic chemical evolution,
formation and evolution first stars, and Type I X-ray burst and
superbursts.
MoCA has very active research groups in Stellar
Interiors and Nucleosynthesis (SINs - Lattanzio, Heger, Campbell,
Mueller), High-energy Astrophysics (Galloway, Levin, Donea, Heger,
Price, Mueller, Lazendic-Galloway, Thrane), Astrophysical Fluid
Dynamics and MHD (Monaghan; Price - star formation), Galaxy Evolution
(Bown), Numerical General Relativity, and solar physics, amongst
others. The initial appointment is for two years, at level A or B
depending on experience. Extension for a third year contingent upon
funding, satisfactory performance, and managment approval.
Commencement date should be on or before Oct. 1, 2015.
To
apply for this post, follow the link provided to the job listing at
Monash. Please arrange for three letters of reference to be sent to
alexander.heger@monash.edu by the closing date.
Attention/Comments:
For full application, please visit Monash web site at
http://jobs.monash.edu.au/jobDetails.asp?sJobIDs=528279
The
application needs to be submitted through the online web
form.
Weblink:
http://jobregister.aas.org/job_view?JobID=49604
Email:
alexander.heger@monash.edu
Deadline: Monday, 1
December 2014, 11:55pm Australian Eastern Daylight Saving Time (early
morning hours in US).
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Rolf Kuiper
Computational Physics
Institute
of Astronomy and Astrophysics Tübingen
University of Tübingen
Auf der Morgenstelle 10
D-72076 Tübingen
Germany
The
Institute of Astronomy and Astrophysics at the University of Tübingen
(IAAT) has an opening for a Postdoc and two PhD positions within the
Emmy Noether Research Group „Accretion flows and feedback in
realistic models of massive star formation“.
The successful
applicants will carry out original research in the field of Massive
Star Formation working in the Emmy Noether group of Dr. Rolf Kuiper.
Emphasis lies on the (radiation-/magneto-)hydrodynamical and chemical
evolution of jets, outflows, and accretion disk around massive
protostars. Applicants with previous experience in numerical modeling
will be favored.
The research activities of the IAAT
(http://www.tat.physik.uni-tuebingen.de) include Astronomy,
Instrumental Design/ High Energy Physics, Computational Astrophysics
and Relativistic Astrophysics. The focus of research of the Emmy
Noether group lies in the field of massive star formation and the
physics/ chemistry of jets, outflows, and accretion disks.
The
appointments are funded by the German Research Foundation (DFG) and
paid according to German public service scale. Starting dates are
negotiable. Applicants should check for details of the application
procedure at links below.
The University of Tübingen seeks to
increase the fraction of female scientists in research and teaching
and particularly encourages applications from women. Disabled
candidates are given preference if equally qualified.
For further
enquires about the positions, please contact Rolf Kuiper
(rolf.kuiper@uni-tuebingen.de).
Attention/Comments:
Weblink: http://www.mpia-hd.mpg.de/~kuiper
Email:
rolf.kuiper@uni-tuebingen.de
Deadline: December,
15th for PhDs and January, 19th for Postdoc
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Alceste Bonanos
IAASARS,
National Observatory of Athens
I. Metaxa & Vas. Pavlou St.
GR-15236, Penteli
Greece
The Institute for Astronomy,
Astrophysics, Sace Applications and Remote Sensing (IAASARS) of the
National Observatory of Athens announces several openings in the
framework of the ESA program "Hubble Catalog of Variables"
and invites applications for the following positions: (i) two
postdoctoral research positions on identifying and characterizing
variable stars in the Hubble Source Catalog; (ii) one postdoctoral
research position with expertise in programming or a software
engineer; (iii) several PhD positions, on projects related to
identifying and characterizing variable stars in the Hubble Source
Catalog (HSC). Applicants with previous experience in stellar
variability (detection algorithms, light curve analysis,
characterization of variables), photometry, HST data or a related
field are particularly encouraged to apply. For more information
visit the link below.
Attention/Comments:
Weblink:
http://www.astro.noa.gr/en/jobopenings/
Email:
bonanos@noa.gr
Deadline: December 15, 2014
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Open JOB offers
Tim Harries
Department of Physics and Astronomy
University of Exeter
Stocker Road
Exeter EX4 4QL
United
Kingdom
The Astrophysics Group at the University of Exeter
invites applications for a postdoctoral position (Associate Research
Fellow / Research Fellow) to work with Tim Harries on radiation
hydrodynamical simulations of massive star formation. This position
is funded by an STFC Consolidated Grant, and is available for 3 years
(subject to a 12-month probationary period).
The main aim of
this project is to investigate the role of radiation pressure and
ionisation feedback on the formation of massive stars. This will be
done using 3-D radiation hydrodynamical models, and by comparing the
simulations with a broad range of multi-wavelength observational
data. We are therefore particularly interested in applicants with a
strong background in radiation transfer and/or hydrodynamics; prior
work on star formation simulations would also be an asset, but all
applicants with a good numerical astrophysics background will be
seriously considered.
Applicants must possess a PhD in
astrophysics or a related discipline, or expect to have earned one
before taking up the position. This position is available from 1st
April 2015, although a later start date may be possible. The starting
salary will range from £25,513 on Grade E to £33,242 per annum on
Grade F, depending on qualifications and experience. Extensive
supercomputing resources and substantial funding for computing
equipment and travel will be available.
For further
information contact Tim Harries (th@astro.ex.ac.uk). Please apply via
the University of Exeter online application system
https://jobs.exeter.ac.uk. The job may be found by searching under
'Key words' using post reference P48022. The closing date for
applications is the 31st January 2015.
Attention/Comments:
Weblink:
http://emps.exeter.ac.uk/physics-astronomy/research/astrophysics/
Email:
th@astro.ex.ac.uk
Deadline: 31st January 2015
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Alexander Heger
Monash Centre for Astrophysics
School of Physics and Astronomy
Monash University, VIC 3800
Australia
Lecturer/Senior Lecturer position in astronomy
or astrophysics at Monash
http://jobs.monash.edu.au/jobDetails.asp?sJobIDs=528830
Applications are invited for a full time Lecturer/Senior
Lecturer (level B/C) in astronomy or astrophysics, in the new School
of Physics and Astronomy at Monash University. This is an opportunity
to join a dynamic, successful and growing School, which encompasses
one of the most diverse astrophysics research groups in Australia.
The role demands a commitment to excellence, innovation and
creativity in research. Applicants will be considered in any of the
School’s current research areas in astronomy and astrophysics.
However, exceptional applicants in other areas of astronomy and
astrophysics are also encouraged to apply.
The successful
candidate will also be expected to contribute to innovative teaching
and learning in the School’s undergraduate astronomy and
astrophysics programmes, including participating in our new "studio
teaching" model through the Physics and Astronomy
Collaborative-learning Environment (PACE). For more information about
the School, visit http://www.physics.monash.edu.au.
To apply
for this position, and for additional information (including complete
position description and selection criteria) visit the job listing at
Monash:
http://jobs.monash.edu.au/jobDetails.asp?sJobIDs=528830
Pre-application enquiries should be directed to Mrs Jean
Pettigrew, Jean.Pettigrew@monash.edu, tel. +61-3 9905
3651.
Attention/Comments:
Weblink:
http://jobregister.aas.org/job_view?JobID=49917
Email:
alexander.heger@monash.edu
Deadline: Sunday, 31
January 2015, 11:55pm Australian Eastern Daylight Time
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Raphael Hirschi
Keele
University
Astrophysics Group
School of Physical and
Geographical Sciences
Lennard-Jones Laboratories
Keele
ST5
5BG, UK
The Astrophysics Group at Keele University has several
funded studentships (STFC/Keele funding) in astronomy/astrophysics to
start in September 2015.
Possible projects include (title,
main supervisor):
- Nuclear astrophysics: impact and sensitivity
studies, Dr Raphael Hirschi
- Nucleosynthesis in rotating stars,
Dr Raphael Hirschi
- Transiting extra-solar planets with
WASP-South, Prof Coel Hellier
- High-precision studies of
eclipsing binary stars observed using space telescopes (Southworth)
- Laboratory astrophysics at the Diamond Light Source, Prof Nye
Evans
- Star formation and stellar ages from the Gaia-ESO
Spectroscopic Survey (Prof. R. D. Jeffries)
- Outer solar system
chemistry (Dr Jacco van Loon, Prof. A. Evans)
- Star formation in
the Magellanic Clouds (Dr. Joana Oliveira)
- Atmospheric
properties of A, F and G stars (Dr Barry Smalley)
Notes:
applications open to EU students (non-EU students can apply for a
self-funded PhD position). More information on the projects, the
Keele astrophysics group and how to apply can be found here:
http://www.keele.ac.uk/researchsubjects/astrophysics/
If you
have questions, please do not hesitate to contact
Dr Raphael
Hirschi
(PhD students coordinator)
Attention/Comments:
Weblink:
http://www.keele.ac.uk/researchsubjects/astrophysics/
Email:
r.hirschi@keele.ac.uk
Deadline: Closing Date 28th
February 2015 (applications received by the deadline will receive
first consideration)
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12 - 14 August 2015
Venue: Honolulu,
Hawaii
A 3-day Focus Meeting entitled "Stellar Physics in
Galaxies throughout the Universe" will be held during the IAU
XXIX General Assembly. The meeting will bring together astronomers
from the stellar physics, extragalactic astrophysics and cosmology
communities to discuss how current and future results can foster
progress in these disjoint science areas. Areas covered include
stellar evolution of single and binary stars from the zero-age
main-sequence to the terminal stage, the feedback of stars to the
interstellar medium via radiation, dust production and chemical
enrichment, and the properties of the most massive stars and of
cosmologically significant stellar phases such as AGB and Wolf-Rayet
stars. We will evaluate the limitations of our understanding of the
physics of local stars and their effects on, e.g., ages, chemical
composition and the initial mass function of galaxies at low to high
redshift. The meeting is timely because of new results from recently
commissioned telescopes and because of the prospects from future 30-m
class telescopes.
Weblink: http://iau-fm7.stsci.edu
Email:
leitherer@stsci.edu
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5-7 May 2015
Venue: Royal Observatory of
Belgium, Brussels, Belgium
Thanks to projects such as the
ongoing Gaia-ESO Survey (GES) and the VLT-Flames Tarantula Survey
(VFTS) progress in the number of massive stars with accurate
parameters is rapidly growing.
In order to bring together the
European expertise in massive-star spectral analysis and evolution it
is timely to organise a Workshop on massive stars in the context of
the Gaia-ESO Survey.
By the time of the meeting about
two-thirds of the GES data will have been collected. The data
reduction and analysis techniques will have been refined to handle
these data and produce significant science output.
One aim of
the workshop is to present the GES results to a wider community of
massive-star experts. The interaction between the various European
massive-star groups will allow us to extract the best science from
the GES data. A second purpose is to interact with the other GES
Co-Is to provide them with the information they need related to e.g.
cluster studies. Finally, it is a timely moment to measure the
progress we have made in achieving the science cases listed in the
GES proposal and to address future directions.
Weblink:
http://ges-ms.oma.be
Email:
Ronny.Blomme@oma.be
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