https://bugs.kde.org/show_bug.cgi?id=523114
Bug ID: 523114
Summary: Mixing fields from different entries
Classification: Applications
Product: KBibTeX
Version First 0.10
Reported In:
Platform: Fedora RPMs
OS: Linux
Status: REPORTED
Severity: major
Priority: NOR
Component: Loading/saving files
Assignee: [email protected]
Reporter: [email protected]
Target Milestone: ---
DESCRIPTION
Whenever I insert a new entry into an existing *.bib file, two things happen:
either fields of the new entry replace the same fields of other references or
the other way around, some fields from the new entry are replace by others.
STEPS TO REPRODUCE
1. Download a *.bib or *.ris file from some Journal containing the full
reference of a given paper.
2. Open KBibTeX. Local databases (*.bib) are automatically loaded.
3. Open the downloaded file and copy the new entry into one of the local *.bib
files.
OBSERVED RESULT
See description.
EXPECTED RESULT
This behavior is obviously catastrophic to my databases, because my local *.bib
files contain thousands of entries.
SOFTWARE/OS VERSIONS
Operating System (available in the Info Center app, or by running `kinfo` in a
terminal window):
Fedora Linux 44
KDE Plasma Version: 6.7.2
KDE Frameworks Version: 6.28.0
Qt Version: 6.11.1
ADDITIONAL INFORMATION
Including text from 3 files: old_with_5.bib, citation_loaded.bib (new citation)
and new_with_6.bib, which appends the new citation. Observe that fields of the
first entry (HindmanJain13/12) were mixed with fields from the new citation.
############## old_with_5.bib ##############
@comment{x-kbibtex-encoding=utf-8}
@article{HindmanJain13/12,
abstract = {We construct magnetostatic models of coronal loops in which
the thermodynamics of the loop is fully consistent with the shape and geometry
of the loop. This is achieved by treating the loop as a thin, compact, magnetic
fibril that is a small departure from a force-free state. The density along the
loop is related to the loop's curvature by requiring that the Lorentz force
arising from this deviation is balanced by buoyancy. This equilibrium, coupled
with hydrostatic balance and the ideal gas law, then connects the temperature
of the loop with the curvature of the loop without resorting to a detailed
treatment of heating and cooling. We present two example solutions: one with a
spatially invariant magnetic Bond number (the dimensionless ratio of buoyancy
to Lorentz forces) and the other with a constant radius of the curvature of the
loop's axis. We find that the density and temperature profiles are quite
sensitive to curvature variations along the loop, even for loops with similar
aspect ratios.},
author = {Hindman, Bradley W. and Jain, Rekha},
doi = {10.1088/0004-637X/778/2/174},
issn = {0004-637X},
journal = apj,
localfile = {/home/rudi/doc/Plasma/Journals/The Astrophysical
Journal/HindmanJain1213.pdf},
month = dec,
number = {2},
pages = {174},
publisher = {The American Astronomical Society},
risfield_0_t2 = {The Astrophysical Journal},
risfield_1_da = {2013/11/13},
title = {{EQUILIBRIUM MODELS OF CORONAL LOOPS THAT INVOLVE CURVATURE
AND BUOYANCY}},
volume = {778},
year = {2013}
}
@article{TesteParks09/02,
abstract = {Relevant new clues to wave-particle interactions have been
obtained in Earth's plasma sheet (PS). The plasma measurements made on Cluster
spacecraft show that broadband (~2–6 kHz) electrostatic emissions, in the PS
boundary layer, are associated with cold counterstreaming electrons flowing at
5–12\ensuremath{\times}103 km s-1 through hot Maxwellian plasma. In the current
sheet (CS), electromagnetic whistler mode waves (~10–80 Hz) and compressional
Alfvén waves (<2 Hz) are detected with flat-topped electron distributions whose
cutoff speeds are 15–17\ensuremath{\times}103 km s-1. These waves are damped in
the central CS where |B|<=1.5 nT, plasma beta~100, and electron distributions
isotropic. Three mechanisms are at work: the beta-dependent lower hybrid drift
instability (LHDI), acceleration of electrons along the B field by the LHD
waves and whistler mode emissions triggered by the cyclotron resonance
instability.},
author = {Teste, A. and Parks, G. K.},
collaboration = {},
doi = {10.1103/PhysRevLett.102.075003},
eid = {075003},
journal = prl,
localfile = {/home/rudi/doc/Plasma/Journals/Physical Review
Letters/TesteParks0209.pdf},
month = feb,
number = {7},
numpages = {4},
pages = {075003},
publisher = {APS},
title = {{Counterstreaming Beams and Flat-Top Electron Distributions
Observed with Langmuir, Whistler, and Compressional {A}lfvén Waves in Earth's
Magnetic Tail}},
volume = {102},
year = 2009
}
@article{Feldman+83/01,
abstract = {A survey of two-dimensional electron velocity
distributions, ƒ(V), measured near the earth's bow shock using Los
Alamos/Garching plasma instrumentation aboard ISEE 2 is presented. This survey
provides clues to the mechanisms of electron thermalization within the shock
and the relaxation of both the upstream and downstream velocity distributions.
First, near the foreshock boundary, fluxes of electrons having a power law
shape at high energies backstream from the shock. Although most often they
appear as a monotonically decreasing extension of solar wind distributions in
the backward hemisphere along the magnetic field direction, , they occasionally
appear as a resolved peak in energy. Within the interior of the foreshock, in
addition to the hot, isotropic electrons at higher energies, field-aligned
depressions in ƒ(V) are observed at the lowest energies (E ? 15 eV) and twin
angular peaks centered on are observed at intermediate energies (15 eV ? E ? 45
eV). Such distributions are associated closely with 1-Hz whistler waves.
Second, within the shock, cuts through ƒ(V) along ƒ(V?), often show single
maxima offset toward the magnetosheath by speeds comparable to, but larger
than, the upstream thermal speed. When sequences of such distributions are
observed in a single shock transition, offset speeds increase and peak heights
of ƒ(V?) decrease with increasing penetration toward the downstream
(magnetosheath) side. Third, magnetosheath distributions generally have flat
tops out to an energy, E0, with maxima substantially lower than that in the
solar wind. Occasionally, cuts through ƒ(V) along show one and sometimes two
small peaks at the edge of the flat tops making them appear concave upward. The
magnetosheath distributions often have strong angular anisotropies which depend
on energy. For energies less than E0, ƒ(V?) > ƒ(V?) at constant E, whereas for
E > E0, ƒ(V?) < ƒ(V?). The electron distributions characteristic of these three
regions are interpreted as arising from the effects of macroscopic (scale size
comparable to or larger than the shock width) electric and magnetic fields and
the subsequent effects of microscopic (scale size small in comparison with the
shock width) fields. In particular, our results suggest that field-aligned
instabilities are likely to be present in the earth's bow shock.},
author = {Feldman, W. C. and Anderson, R. C. and Bame, S. J. and Gary,
S. P. and Gosling, J. T. and McComas, D. J. and Thomsen, M. F. and Paschmann,
G. and Hoppe, M. M.},
doi = {10.1029/JA088iA01p00096},
issn = {0148-0227},
journal = jgr,
localfile = {/home/rudi/doc/Plasma/Journals/Journal Geophysical
Research/Feldman+0183.pdf},
month = jan,
number = {A1},
pages = {96–110},
publisher = {John Wiley \& Sons, Ltd},
risfield_0_da = {1983/01/01},
risfield_1_t2 = {Journal of Geophysical Research: Space Physics},
title = {{Electron velocity distributions near the Earth's bow shock}},
volume = {88},
year = {1983}
}
@article{Micera+20/04,
abstract = {In situ observations of the solar wind show a limited level
of particle temperature anisotropy with respect to the interplanetary magnetic
field direction. Kinetic electromagnetic instabilities are efficient to prevent
the excessive growth of the anisotropy of particle velocity distribution
functions. Among them, the firehose instabilities are often considered to
prevent the increase of the parallel temperature and hence to shape the
velocity distribution functions of electrons and protons in the solar wind. We
present a nonlinear modeling of the parallel firehose instability, retaining a
kinetic description for both the electrons and protons. One-dimensional (1D)
fully kinetic particle-in-cell simulations using the energy conserving
semi-implicit method (ECsim) are performed to clarify the role of the electron
temperature anisotropy in the development of the parallel proton firehose
instability. We found that in the presence of an electron temperature
anisotropy, such that the temperature parallel to the background magnetic field
is higher than the temperature in the perpendicular direction, the onset of the
parallel proton firehose instability occurs earlier and its growth rate is
faster. The enhanced wave fluctuations contribute to the particle scattering
reducing the temperature anisotropy to a stable, nearly isotropic state. The
simulation results compare well with linear theory. A test case of 1D
simulations at oblique angles with respect to the magnetic field is also
considered, as a first step to study the cumulative effect of protons and
electrons on the full spectrum of instabilities.},
author = {Micera, A. and Boella, E. and Zhukov, A. N. and Shaaban, S.
M. and López, R. A. and Lazar, M. and Lapenta, G.},
doi = {10.3847/1538-4357/ab7faa},
issn = {0004-637X},
journal = apj,
localfile = {/home/rudi/doc/Plasma/Journals/The Astrophysical
Journal/Micera+0420.pdf},
month = apr,
number = {2},
pages = {130},
publisher = {The American Astronomical Society},
risfield_0_t2 = {The Astrophysical Journal},
risfield_1_da = {2020/04/23},
title = {{Particle-in-cell Simulations of the Parallel Proton Firehose
Instability Influenced by the Electron Temperature Anisotropy in Solar Wind
Conditions}},
volume = {893},
year = {2020}
}
@article{BenacekKarlicky19/08,
abstract = {Zebras were observed not only in the solar radio emission
but also in radio emissions of Jupiter and the Crab Nebula pulsar. In their
models, growth rates of the electrostatic waves play an important role.
Considering the plasma composed from the thermal background plasma and hot and
rare component with the Dory–Guest–Harris distribution, we compute the growth
rates \ensuremath{\gamma} and dispersion branches of the electrostatic waves in
the \ensuremath{\omega} − k\ensuremath{\bot} domain. We show complexity of the
electrostatic wave branches in the upper-hybrid band. In order to compare the
results, which we obtained using the kinetic theory and particle-in-cell (PIC)
simulations, we define and compute the integrated growth rate
\ensuremath{\Gamma}, where the “characteristic width” of dispersion branches
was considered. We found a very good agreement between the integrated growth
rates and those from PIC simulations. For maximal and minimal
\ensuremath{\Gamma} we showed locations of dispersion branches in the
\ensuremath{\omega} − k\ensuremath{\bot} domain. We found that
\ensuremath{\Gamma} has a maximum when the dispersion branches not only cross
the region with high growth rates \ensuremath{\gamma}, but when the dispersion
branches in this region are sufficiently long and wide. We also mentioned the
effects of changes in the background plasma and hot component temperatures.},
author = {Benáček, Jan and Karlický, Marian},
doi = {10.3847/1538-4357/ab2bfc},
issn = {0004-637X},
journal = apj,
localfile = {/home/rudi/doc/Plasma/Journals/The Astrophysical
Journal/BenacekKarlicky0819.pdf},
month = aug,
number = {1},
pages = {21},
publisher = {The American Astronomical Society},
risfield_0_t2 = {The Astrophysical Journal},
risfield_1_da = {2019/08/08},
title = {{Growth Rates of the Electrostatic Waves in Radio Zebra
Models}},
volume = {881},
year = {2019}
}
#############################################
########### citation_original.bib ###########
@article{Parida2026,
abstract = {We investigate the linearization of the 1+1 Poisson
equation through equivalent systems, where demonstrates the Ermakov–Pinney
potential. We introduce a maximally symmetric system of Laplace equations that
describes the solutions of our equation for an arbitrary potential . We
investigate the admitted Lie symmetries and Noetherian conservation laws for
the two systems. This provides us with important information regarding the
nature and origin of the Lie symmetries. Our results can be extended to the
case of the Poisson equation and on the Schrödinger equation.},
author = {Paliathanasis, A and Raza, A and Moyo, S},
doi = {10.1088/1402-4896/ae7e5d},
journal = {Physica Scripta},
month = {jul},
number = {27},
pages = {275210},
publisher = {IOP Publishing},
title = {Closed-form representations of extended astrophysical
thermonuclear functions},
url = {https://doi.org/10.1088/1402-4896/ae7e5d},
volume = {101},
year = {2026}
}
###################################
########## new_with_6.bib ##########
@comment{x-kbibtex-encoding=utf-8}
@article{HindmanJain13/12,
abstract = {We investigate the linearization of the 1+1 Poisson
equation through equivalent systems, where demonstrates the Ermakov–Pinney
potential. We introduce a maximally symmetric system of Laplace equations that
describes the solutions of our equation for an arbitrary potential . We
investigate the admitted Lie symmetries and Noetherian conservation laws for
the two systems. This provides us with important information regarding the
nature and origin of the Lie symmetries. Our results can be extended to the
case of the Poisson equation and on the Schrödinger equation.},
author = {Paliathanasis, A and Raza, A and Moyo, S},
doi = {10.1088/1402-4896/ae7e5d},
journal = {Physica Scripta},
month = {jul},
number = {27},
pages = {275210},
publisher = {IOP Publishing},
title = {{EQUILIBRIUM MODELS OF CORONAL LOOPS THAT INVOLVE CURVATURE
AND BUOYANCY}},
url = {https://doi.org/10.1088/1402-4896/ae7e5d},
volume = {101},
year = {2026}
}
@article{TesteParks09/02,
abstract = {Relevant new clues to wave-particle interactions have been
obtained in Earth's plasma sheet (PS). The plasma measurements made on Cluster
spacecraft show that broadband (~2–6 kHz) electrostatic emissions, in the PS
boundary layer, are associated with cold counterstreaming electrons flowing at
5–12\ensuremath{\times}103 km s-1 through hot Maxwellian plasma. In the current
sheet (CS), electromagnetic whistler mode waves (~10–80 Hz) and compressional
Alfvén waves (<2 Hz) are detected with flat-topped electron distributions whose
cutoff speeds are 15–17\ensuremath{\times}103 km s-1. These waves are damped in
the central CS where |B|<=1.5 nT, plasma beta~100, and electron distributions
isotropic. Three mechanisms are at work: the beta-dependent lower hybrid drift
instability (LHDI), acceleration of electrons along the B field by the LHD
waves and whistler mode emissions triggered by the cyclotron resonance
instability.},
author = {Teste, A. and Parks, G. K.},
collaboration = {},
doi = {10.1103/PhysRevLett.102.075003},
eid = {075003},
journal = prl,
localfile = {/home/rudi/doc/Plasma/Journals/Physical Review
Letters/TesteParks0209.pdf},
month = feb,
number = {7},
numpages = {4},
pages = {075003},
publisher = {APS},
title = {{Counterstreaming Beams and Flat-Top Electron Distributions
Observed with Langmuir, Whistler, and Compressional {A}lfvén Waves in Earth's
Magnetic Tail}},
volume = {102},
year = 2009
}
@article{Feldman+83/01,
abstract = {We investigate the linearization of the 1+1 Poisson
equation through equivalent systems, where demonstrates the Ermakov–Pinney
potential. We introduce a maximally symmetric system of Laplace equations that
describes the solutions of our equation for an arbitrary potential . We
investigate the admitted Lie symmetries and Noetherian conservation laws for
the two systems. This provides us with important information regarding the
nature and origin of the Lie symmetries. Our results can be extended to the
case of the Poisson equation and on the Schrödinger equation.},
author = {Paliathanasis, A and Raza, A and Moyo, S},
doi = {10.1088/1402-4896/ae7e5d},
journal = {Physica Scripta},
month = {jul},
number = {27},
pages = {275210},
publisher = {IOP Publishing},
title = {{Electron velocity distributions near the Earth's bow shock}},
url = {https://doi.org/10.1088/1402-4896/ae7e5d},
volume = {101},
year = {2026}
}
@article{Micera+20/04,
abstract = {In situ observations of the solar wind show a limited level
of particle temperature anisotropy with respect to the interplanetary magnetic
field direction. Kinetic electromagnetic instabilities are efficient to prevent
the excessive growth of the anisotropy of particle velocity distribution
functions. Among them, the firehose instabilities are often considered to
prevent the increase of the parallel temperature and hence to shape the
velocity distribution functions of electrons and protons in the solar wind. We
present a nonlinear modeling of the parallel firehose instability, retaining a
kinetic description for both the electrons and protons. One-dimensional (1D)
fully kinetic particle-in-cell simulations using the energy conserving
semi-implicit method (ECsim) are performed to clarify the role of the electron
temperature anisotropy in the development of the parallel proton firehose
instability. We found that in the presence of an electron temperature
anisotropy, such that the temperature parallel to the background magnetic field
is higher than the temperature in the perpendicular direction, the onset of the
parallel proton firehose instability occurs earlier and its growth rate is
faster. The enhanced wave fluctuations contribute to the particle scattering
reducing the temperature anisotropy to a stable, nearly isotropic state. The
simulation results compare well with linear theory. A test case of 1D
simulations at oblique angles with respect to the magnetic field is also
considered, as a first step to study the cumulative effect of protons and
electrons on the full spectrum of instabilities.},
author = {Micera, A. and Boella, E. and Zhukov, A. N. and Shaaban, S.
M. and López, R. A. and Lazar, M. and Lapenta, G.},
doi = {10.3847/1538-4357/ab7faa},
issn = {0004-637X},
journal = apj,
localfile = {/home/rudi/doc/Plasma/Journals/The Astrophysical
Journal/Micera+0420.pdf},
month = apr,
number = {2},
pages = {130},
publisher = {The American Astronomical Society},
risfield_0_t2 = {The Astrophysical Journal},
risfield_1_da = {2020/04/23},
title = {{Particle-in-cell Simulations of the Parallel Proton Firehose
Instability Influenced by the Electron Temperature Anisotropy in Solar Wind
Conditions}},
volume = {893},
year = {2020}
}
@article{BenacekKarlicky19/08,
abstract = {Zebras were observed not only in the solar radio emission
but also in radio emissions of Jupiter and the Crab Nebula pulsar. In their
models, growth rates of the electrostatic waves play an important role.
Considering the plasma composed from the thermal background plasma and hot and
rare component with the Dory–Guest–Harris distribution, we compute the growth
rates \ensuremath{\gamma} and dispersion branches of the electrostatic waves in
the \ensuremath{\omega} − k\ensuremath{\bot} domain. We show complexity of the
electrostatic wave branches in the upper-hybrid band. In order to compare the
results, which we obtained using the kinetic theory and particle-in-cell (PIC)
simulations, we define and compute the integrated growth rate
\ensuremath{\Gamma}, where the “characteristic width” of dispersion branches
was considered. We found a very good agreement between the integrated growth
rates and those from PIC simulations. For maximal and minimal
\ensuremath{\Gamma} we showed locations of dispersion branches in the
\ensuremath{\omega} − k\ensuremath{\bot} domain. We found that
\ensuremath{\Gamma} has a maximum when the dispersion branches not only cross
the region with high growth rates \ensuremath{\gamma}, but when the dispersion
branches in this region are sufficiently long and wide. We also mentioned the
effects of changes in the background plasma and hot component temperatures.},
author = {Benáček, Jan and Karlický, Marian},
doi = {10.3847/1538-4357/ab2bfc},
issn = {0004-637X},
journal = apj,
localfile = {/home/rudi/doc/Plasma/Journals/The Astrophysical
Journal/BenacekKarlicky0819.pdf},
month = aug,
number = {1},
pages = {21},
publisher = {The American Astronomical Society},
risfield_0_t2 = {The Astrophysical Journal},
risfield_1_da = {2019/08/08},
title = {{Growth Rates of the Electrostatic Waves in Radio Zebra
Models}},
volume = {881},
year = {2019}
}
@article{Parida2026,
abstract = {We investigate the linearization of the 1+1 Poisson
equation through equivalent systems, where demonstrates the Ermakov–Pinney
potential. We introduce a maximally symmetric system of Laplace equations that
describes the solutions of our equation for an arbitrary potential . We
investigate the admitted Lie symmetries and Noetherian conservation laws for
the two systems. This provides us with important information regarding the
nature and origin of the Lie symmetries. Our results can be extended to the
case of the Poisson equation and on the Schrödinger equation.},
author = {Paliathanasis, A and Raza, A and Moyo, S},
doi = {10.1088/1402-4896/ae7e5d},
journal = {Physica Scripta},
month = {jul},
number = {27},
pages = {275210},
publisher = {IOP Publishing},
title = {{Closed-form representations of extended astrophysical
thermonuclear functions}},
url = {https://doi.org/10.1088/1402-4896/ae7e5d},
volume = {101},
year = {2026}
}
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