114 research outputs found
Characterization of Cg10062 from Corynebacterium glutamicum: Implications for the Evolution of cis-3-Chloroacrylic Acid Dehalogenase Activity in the Tautomerase Superfamily†
A 149-amino acid protein designated Cg10062 is encoded by a gene from Corynebacterium glutamicum. The physiological function of Cg10062 is unknown, and the gene encoding this protein has no obvious genomic context. Sequence analysis links Cg10062 to the cis-3-chloroacrylic acid dehalogenase (cis-CaaD) family, one of the five known families of the tautomerase superfamily. The characterized tautomerase superfamily members have two distinctive characteristics: a P-cc-p structure motif and a catalytic amino-terminal proline. Pro-1 is present in the Cg10062 amino acid sequence along with His-28, Arg-70, Arg-73, Tyr-103, and Glu-114, all of which have been implicated as critical residues for cis-CaaD activity. The gene for Cg10062 has been cloned and the protein overproduced, purified, and subjected to kinetic and mechanistic characterization. Like cis-CaaD, Cg10062 functions as a hydratase: it converts 2-oxo-3-pentynoate to acetopyruvate and processes 3-bromopropiolate to a species that inactivates the enzyme by acylation of Pro-1. Kinetic and (1)H NMR spectroscopic studies also show that Cg10062 processes both isomers of 3-chloroacrylic acid at low levels with a clear preference for the cis isomer. Pro-1 is critical for the dehalogenase and hydratase activities because the PIA mutant no longer catalyzes either reaction. The presence of the six key catalytic residues and the hydratase activity coupled with the absence of an efficient cis-CaaD activity and the lack of isomer specificity implicate factors beyond this core set of residues in cis-CaaD catalysis and specificity. This work sets the stage for in-depth mechanistic and structural studies of Cg10062, which could identify the additional features necessary for a fully active and highly specific cis-CaaD. Such results will also shed light on how cis-CaaD emerged in the tautomerase superfamily because Cg10062 could be characteristic of an intermediate along the evolutionary pathway for this dehalogenase
Inactivation of Cg10062, a cis-3-Chloroacrylic Acid Dehalogenase Homologue in Corynebacterium glutamicum, by (R)- and (S)-Oxirane-2-carboxylate: Analysis and Implications
Thermohaline mixing in low-mass giants: RGB and beyond
Thermohaline mixing has recently been proposed to occur in low mass red
giants, with large consequence for the chemical yields of low mass stars. We
investigate the role of thermohaline mixing during the evolution of stars
between 1 Msun and 3 Msun. We use a stellar evolution code which includes
rotational mixing and internal magnetic fields. We confirm that thermohaline
mixing has the potential to destroy most of the helium 3 which is produced
earlier on the main sequence during the red giant stage, in stars below
1.5Msun. We find this process to continue during core helium burning and
beyond. We find rotational and magnetic mixing to be negligible compared to the
thermohaline mixing in the relevant layers, even if the interaction of
thermohaline motions with the differential rotation may be essential to
establish the time scale of thermohaline mixing in red giants.Comment: Proceedings of the Conference "Unsolved problems in stellar physics"
- Cambridge, July 200
Goede diergezondheid mogelijk bij scherp voeren
De eerste indruk is dat ook bij scherp letten op stikstof en fosfaat de diergezondheid goed kan zijn
The Effects of Binary Evolution on the Dynamics of Core Collapse and Neutron-Star Kicks
We systematically examine how the presence in a binary affects the final core
structure of a massive star and its consequences for the subsequent supernova
explosion. Interactions with a companion star may change the final rate of
rotation, the size of the helium core, the strength of carbon burning and the
final iron core mass. Stars with initial masses larger than \sim 11\Ms that
experiece core collapse will generally have smaller iron cores at the time of
the explosion if they lost their envelopes due to a previous binary
interaction. Stars below \sim 11\Ms, on the other hand, can end up with larger
helium and metal cores if they have a close companion, since the second
dredge-up phase which reduces the helium core mass dramatically in single stars
does not occur once the hydrogen envelope is lost. We find that the initially
more massive stars in binary systems with masses in the range 8 - 11\Ms are
likely to undergo an electron-capture supernova, while single stars in the same
mass range would end as ONeMg white dwarfs. We suggest that the core collapse
in an electron-capture supernova (and possibly in the case of relatively small
iron cores) leads to a prompt explosion rather than a delayed neutrino-driven
explosion and that this naturally produces neutron stars with low-velocity
kicks. This leads to a dichotomous distribution of neutron star kicks, as
inferred previously, where neutron stars in relatively close binaries attain
low kick velocities. We illustrate the consequences of such a dichotomous kick
scenario using binary population synthesis simulations and discuss its
implications. This scenario has also important consequences for the minimum
initial mass of a massive star that becomes a neutron star. (Abbreviated.)Comment: 8 pages, 3 figures, submitted to ApJ, updated versio
Routekaart biodiversiteit : aanbevelingen voor de aanpak van biodiversiteit binnen de zuivelketen
The Dutch dairy sector is working on improving sustainability. Improving biodiversity is a part of this effort. This report describes the results of research focused on how dairy farms can contribute to biodiversity, the attitude of farmers towards sustainability targets and opportunities to work on future biodiversity goals. The final results in the report are recommendations for the Dutch dairy chain partners to come to a biodiversity implementation plan for dairy farms. The recommendations are focused on designing a farm oriented system to work on biodiversity, on increasing the knowledge about the soil-plant-system-approach and to work on a targeted communication strategy on biodiversity
Impact of eV-mass sterile neutrinos on neutrino-driven supernova outflows
Motivated by recent hints for sterile neutrinos from the reactor anomaly, we
study active-sterile conversions in a three-flavor scenario (2 active + 1
sterile families) for three different representative times during the
neutrino-cooling evolution of the proto-neutron star born in an
electron-capture supernova. In our "early model" (0.5 s post bounce), the
nu_e-nu_s MSW effect driven by Delta m^2=2.35 eV^2 is dominated by ordinary
matter and leads to a complete nu_e-nu_s swap with little or no trace of
collective flavor oscillations. In our "intermediate" (2.9 s p.b.) and "late
models" (6.5 s p.b.), neutrinos themselves significantly modify the nu_e-nu_s
matter effect, and, in particular in the late model, nu-nu refraction strongly
reduces the matter effect, largely suppressing the overall nu_e-nu_s MSW
conversion. This phenomenon has not been reported in previous studies of
active-sterile supernova neutrino oscillations. We always include the feedback
effect on the electron fraction Y_e due to neutrino oscillations. In all
examples, Y_e is reduced and therefore the presence of sterile neutrinos can
affect the conditions for heavy-element formation in the supernova ejecta, even
if probably not enabling the r-process in the investigated outflows of an
electron-capture supernova. The impact of neutrino-neutrino refraction is
strong but complicated, leaving open the possibility that with a more complete
treatment, or for other supernova models, active-sterile neutrino oscillations
could generate conditions suitable for the r-process.Comment: 23 pages, including 14 figures and 2 tables (minor changes in the
text). Matches published version in JCA
Multi-telescope timing of PSR J1518+4904
PSR J1518+4904 is one of only 9 known double neutron star systems. These
systems are highly valuable for measuring the masses of neutron stars,
measuring the effects of gravity, and testing gravitational theories. We
determine an improved timing solution for a mildly relativistic double neutron
star system, combining data from multiple telescopes. We set better constraints
on relativistic parameters and the separate masses of the system, and discuss
the evolution of PSR J1518+4904 in the context of other double neutron star
systems. PSR J1518+4904 has been regularly observed for more than 10 years by
the European Pulsar Timing Array (EPTA) network using the Westerbork, Jodrell
Bank, Effelsberg and Nancay radio telescopes. The data were analysed using the
updated timing software Tempo2. We have improved the timing solution for this
double neutron star system. The periastron advance has been refined and a
significant detection of proper motion is presented. It is not likely that more
post-Keplerian parameters, with which the individual neutron star masses and
the inclination angle of the system can be determined separately, can be
measured in the near future. Using a combination of the high-quality data sets
present in the EPTA collaboration, extended with the original GBT data, we have
constrained the masses in the system to m_p1.55 msun (95.4%
confidence), and the inclination angle of the orbit to be less than 47 degrees
(99%). From this we derive that the pulsar in this system possibly has one of
the lowest neutron star masses measured to date. From evolutionary
considerations it seems likely that the companion star, despite its high mass,
was formed in an electron-capture supernova.Comment: 11 pages, 8 figures, accepted by A&
Proton Motive Force-Dependent Hoechst 33342 Transport by the ABC Transporter LmrA of Lactococcus lactis
The fluorescent compound Hoechst 33342 is a substrate for many multidrug resistance (MDR) transporters and is widely used to characterize their transport activity. We have constructed mutants of the adenosine triphosphate (ATP) binding cassette (ABC)-type MDR transporter LmrA of Lactococcus lactis that are defective in ATP hydrolysis. These mutants and wild-type LmrA exhibited an atypical behavior in the Hoechst 33342 transport assay. In membrane vesicles, Hoechst 33342 transport was shown to be independent of the ATPase activity of LmrA, and it was not inhibited by orthovanadate but sensitive to uncouplers that collapse the proton gradient and to N,N'-dicyclohexylcarbodiimide, an inhibitor of the F0F1-ATPase. In contrast, transport of Hoechst 33342 by the homologous, heterodimeric MDR transporter LmrCD showed a normal ATP dependence and was insensitive to uncouplers of the proton gradient. With intact cells, expression of LmrA resulted in an increased rate of Hoechst 33342 influx while LmrCD caused a decrease in the rate of Hoechst 33342 influx. Cellular toxicity assays using a triple knockout strain, i.e., L. lactis ΔlmrA ΔlmrCD, demonstrate that expression of LmrCD protects cells against the growth inhibitory effects of Hoechst 33342, while in the presence of LmrA, cells are more susceptible to Hoechst 33342. Our data demonstrate that the LmrA-mediated Hoechst 33342 transport in membrane vesicles is influenced by the transmembrane pH gradient due to a pH-dependent partitioning of Hoechst 33342 into the membrane.
Evolution of the number of accreting white dwarfs with shell nuclear burning and of occurrence rate of SN Ia
We analyze temporal evolution of the number of accreting white dwarfs with
shell hydrogen burning in semidetached and detached binaries. We consider a
stellar system in which star formation lasts for 10 Gyr with a constant rate,
as well as a system in which the same amount of stars is formed in a single
burst lasting for 1 Gyr. Evolution of the number of white dwarfs is confronted
to the evolution of occurrence rate of events that usually are identified with
SN Ia or accretion-induced collapses, i.e. with accumulation of Chandrasekhar
mass by a white dwarf or a merger of a pair of CO white dwarfs with total mass
not lower than the Chandrasekhar one. In the systems with a burst of star
formation, at 10 Gyr observed supersoft X-ray sources, most probably, are
not precursors of SN Ia. The same is true for an overwhelming majority of the
sources in the systems with constant star formation rate. In the systems of
both kinds mergers of white dwarfs is the dominant SN Ia scenario. In symbiotic
binaries, accreting CO-dwarfs do not accumulate enough mass for SN Ia
explosion, while ONeMg-dwarfs finish their evolution by an accretion-induced
collapse with formation of a neutron star.Comment: 11 pages, 2 figures, accepted by Astronomy Letter
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