41 research outputs found
Investigating magnetic activity in very stable stellar magnetic fields: long-term photometric and spectroscopic study of the fully convective M4 dwarf V374 Peg
The ultrafast-rotating () fully convective
single M4 dwarf V374 Peg is a well-known laboratory for studying intense
stellar activity in a stable magnetic topology. As an observable proxy for the
stellar magnetic field, we study the stability of the light curve, and thus the
spot configuration. We also measure the occurrence rate of flares and coronal
mass ejections (CMEs). We analyse spectroscopic observations,
photometry covering 5 years, and additional photometry that expands the
temporal base over 16 years. The light curve suggests an almost rigid-body
rotation, and a spot configuration that is stable over about 16 years,
confirming the previous indications of a very stable magnetic field. We
observed small changes on a nightly timescale, and frequent flaring, including
a possible sympathetic flare. The strongest flares seem to be more concentrated
around the phase where the light curve indicates a smaller active region.
Spectral data suggest a complex CME with falling-back and re-ejected material,
with a maximal projected velocity of 675km/s. We observed a CME rate
much lower than expected from extrapolations of the solar flare-CME relation to
active stars.Comment: 15 figures, 4 tables, accepted for publication in A&
The UV surface habitability of Proxima <i>b</i>: first experiments revealing probable life survival to stellar flares
Abstract We use a new interdisciplinary approach to study the UV surface habitability of Proxima b under quiescent and flaring stellar conditions. We assumed planetary atmospheric compositions based on CO2 and N2 and surface pressures from 100 to 5000 mbar. Our results show that the combination of these atmospheric compositions and pressures provide enough shielding from the most damaging UV wavelengths, expanding the ”UV-protective” planetary atmospheric compositions beyond ozone. Additionally, we show that the UV radiation reaching the surface of Proxima b during quiescent conditions would be negligible from the biological point of view, even without an atmosphere. Given that high UV fluxes could challenge the existence of life, then, we experimentally tested the effect that flares would have on microorganisms in a ”worst case scenario” (no UV-shielding). Our results show the impact that a typical flare and a superflare would have on life: when microorganisms receive very high fluences of UVC, such as those expected to reach the surface of Proxima b after a typical flare or a superflare, a fraction of the population is able to survive. Our study suggests that life could cope with highly UV irradiated environments in exoplanets under conditions that cannot be found on Earth
Investigating magnetic activity in very stable stellar magnetic fields: Long-term photometric and spectroscopic study of the fully convective M4 dwarf V374 Pegasi
The ultrafast-rotating (Prot ≈ 0.44 d) fully convective single M4 dwarf V374 Peg is a well-known laboratory for studying intense stellar activity in a stable magnetic topology. As an observable proxy for the stellar magnetic field, we study the stability of the light curve, hence the spot configuration. We also measure the occurrence rate of flares and coronal mass ejections (CMEs). We have analysed spectroscopic observations, BV(RI)C photometry covering 5 yrs, and additional RC photometry that expands the temporal base over 16 yr. The light curve suggests an almost rigid-body rotation and a spot configuration that is stable over about 16 yrs, confirming the previous indications of a very stable magnetic field. We observed small changes on a nightly timescale and frequent flaring, including a possible sympathetic flare. The strongest flares seem to be more concentrated around the phase where the light curve indicates a smaller active region. Spectral data suggest a complex CME with falling-back and re-ejected material with a maximal projected velocity of ~675 km s-1. We observed a CME rate that is much lower than expected from extrapolations of the solar flare-CME relation to active stars. </p
A Helicity-Based Method to Infer the CME Magnetic Field Magnitude in Sun and Geospace: Generalization and Extension to Sun-Like and M-Dwarf Stars and Implications for Exoplanet Habitability
Patsourakos et al. (Astrophys. J. 817, 14, 2016) and Patsourakos and
Georgoulis (Astron. Astrophys. 595, A121, 2016) introduced a method to infer
the axial magnetic field in flux-rope coronal mass ejections (CMEs) in the
solar corona and farther away in the interplanetary medium. The method, based
on the conservation principle of magnetic helicity, uses the relative magnetic
helicity of the solar source region as input estimates, along with the radius
and length of the corresponding CME flux rope. The method was initially applied
to cylindrical force-free flux ropes, with encouraging results. We hereby
extend our framework along two distinct lines. First, we generalize our
formalism to several possible flux-rope configurations (linear and nonlinear
force-free, non-force-free, spheromak, and torus) to investigate the dependence
of the resulting CME axial magnetic field on input parameters and the employed
flux-rope configuration. Second, we generalize our framework to both Sun-like
and active M-dwarf stars hosting superflares. In a qualitative sense, we find
that Earth may not experience severe atmosphere-eroding magnetospheric
compression even for eruptive solar superflares with energies ~ 10^4 times
higher than those of the largest Geostationary Operational Environmental
Satellite (GOES) X-class flares currently observed. In addition, the two
recently discovered exoplanets with the highest Earth-similarity index, Kepler
438b and Proxima b, seem to lie in the prohibitive zone of atmospheric erosion
due to interplanetary CMEs (ICMEs), except when they possess planetary magnetic
fields that are much higher than that of Earth.Comment: http://adsabs.harvard.edu/abs/2017SoPh..292...89
Failure or success? Defensive strategies and piecemeal change among racial inequalities in the Brazilian banking sector
We analyze how Brazilian Black Movement organizations and banks deployed different mechanisms like cooperation, cooptation, and confrontation that generated affirmative action initiatives in the banking sector at the beginning of this century. Black movement organizations triggered an institutional change by connecting fields and exploring a constellation of strategies. However, Brazilian banks adopted defensive strategies aiming to accommodate their interests. We find that only piecemeal change occurred, as the field’s structures – resource distribution and power – remained unscratched. We conclude by noting how the success of social movement strategies can depend upon the framing and sense-giving work that social movements conduct in their continuous jockeying activity toward incumbents
Future mmVLBI Research with ALMA: A European vision
Very long baseline interferometry at millimetre/submillimetre wavelengths
(mmVLBI) offers the highest achievable spatial resolution at any wavelength in
astronomy. The anticipated inclusion of ALMA as a phased array into a global
VLBI network will bring unprecedented sensitivity and a transformational leap
in capabilities for mmVLBI. Building on years of pioneering efforts in the US
and Europe the ongoing ALMA Phasing Project (APP), a US-led international
collaboration with MPIfR-led European contributions, is expected to deliver a
beamformer and VLBI capability to ALMA by the end of 2014 (APP: Fish et al.
2013, arXiv:1309.3519).
This report focuses on the future use of mmVLBI by the international users
community from a European viewpoint. Firstly, it highlights the intense science
interest in Europe in future mmVLBI observations as compiled from the responses
to a general call to the European community for future research projects. A
wide range of research is presented that includes, amongst others:
- Imaging the event horizon of the black hole at the centre of the Galaxy
- Testing the theory of General Relativity an/or searching for alternative
theories
- Studying the origin of AGN jets and jet formation
- Cosmological evolution of galaxies and BHs, AGN feedback
- Masers in the Milky Way (in stars and star-forming regions)
- Extragalactic emission lines and astro-chemistry
- Redshifted absorption lines in distant galaxies and study of the ISM and
circumnuclear gas
- Pulsars, neutron stars, X-ray binaries
- Testing cosmology
- Testing fundamental physical constantsComment: Replaced figures 2 and 3: corrected position SRT. Corrected minor
typo in 5.
Protective effects of halite to vacuum and vacuum-ultraviolet radiation: A potential scenario during a young sun superflare
Halite (NaCl mineral) has exhibited the potential to preserve microorganisms for millions of years on Earth. This mineral was also identified on Mars and in meteorites. In this study, we investigated the potential of halite crystals to protect microbial life-forms on the surface of an airless body (e.g., meteorite), for instance, during a lithopanspermia process (interplanetary travel step) in the early Solar System. To investigate the effect of the radiation of the young Sun on microorganisms, we performed extensive simulation experiments by employing a synchrotron facility. We focused on two exposure conditions: vacuum (low Earth orbit, 10-4 Pa) and vacuum-ultraviolet (VUV) radiation (range 57.6-124 nm, flux 7.14 W/m2), with the latter representing an extreme scenario with high VUV fluxes comparable to the amount of radiation of a stellar superflare from the young Sun. The stellar VUV parameters were estimated by using the very well-studied solar analog of the young Sun, κ1 Cet. To evaluate the protective effects of halite, we entrapped a halophilic archaeon (Haloferax volcanii) and a non-halophilic bacterium (Deinococcus radiodurans) in laboratory-grown halite. Control groups were cells entrapped in salt crystals (mixtures of different salts and NaCl) and non-trapped (naked) cells, respectively. All groups were exposed either to vacuum alone or to vacuum plus VUV. Our results demonstrate that halite can serve as protection against vacuum and VUV radiation, regardless of the type of microorganism. In addition, we found that the protection is higher than provided by crystals obtained from mixtures of salts. This extends the protective effects of halite documented in previous studies and reinforces the possibility to consider the crystals of this mineral as potential preservation structures in airless bodies or as vehicles for the interplanetary transfer of microorganisms.X.C.A. acknowledges CNPEM for the beamtime grantedto the proposal TGM—16126 (LNLS), FAPESP postdoc-toral fellowship (years 2013–2014) (Processo nro: 2012/20106-5), Brazil, and funding from PIP—CONICET 0754,Argentina. M.L. and P.O. acknowledge the Austrian ScienceFund (FWF): P30949-N36, I5711-N for supporting thisproject. J.E.H. acknowledges the financial support of FAPESP (Sao Paulo State) and CNPQ (Brazil) financingagencies. G.F.P.M. acknowledges grant 474972/2009-7from CNPq/Brazil.Peer reviewe
Geophysical and atmospheric evolution of habitable planets
The evolution of Earth-like habitable planets is a complex process that depends on the geodynamical and geophysical environments. In particular, it is necessary that plate tectonics remain active over billions of years. These geophysically active environments are strongly coupled to a planet's host star parameters, such as mass, luminosity and activity, orbit location of the habitable zone, and the planet's initial water inventory. Depending on the host star's radiation and particle flux evolution, the composition in the thermosphere, and the availability of an active magnetic dynamo, the atmospheres of Earth-like planets within their habitable zones are differently affected due to thermal and nonthermal escape processes. For some planets, strong atmospheric escape could even effect the stability of the atmosphere
Dynamics of solar mesogranulation
Using a 45.5-h time series of photospheric flow fields
generated from a set of
high-resolution continuum images (SOHO/MDI) we analyze the
dynamics of solar mesogranule features. The series was prepared
applying a local correlation tracking algorithm with
a 4.8´´ FWHM window. By computing 1-h running means in time
steps of 10 min we generate 267 averaged divergence maps that
are segmented to obtain binary maps. A tracking algorithm
determines lifetimes and barycenter coordinates of
regions of positive divergence defined as mesogranules (MGs).
If we analyze features of lifetimes ≥1 h and
of areas ≥5 Mm we find a mean drift velocity of
304 m s-1 (with ± variation of 180 m s-1), a mean
travel distance of Mm, a mean lifetime of
h, and a decay time of 1.6 h for
a total of 2022 MGs. The advective motion of MGs
within supergranules is seen for 50 to 70% of the long-lived
(≥4 h) MGs while the short-lived ones move irregularly.
If only the long-lived MGs are further analyzed
the drift velocities reduce to 207 m s-1 and the
travel distances increase to 4.1 Mm on average,
which is an appreciable fraction of the supergranular radius.
The results are largely independent of the divergence
segmentation level.