Second-order Cosmological Perturbations Engendered by Point-like MassesMaxim Eingorn
R. Brilenkov and M. Eingorn, Second-order cosmological perturbations engendered by point-like masses, ApJ 845 (2017) 153: http://iopscience.iop.org/article/10.3847/1538-4357/aa81cd
In the ΛCDM framework, presenting nonrelativistic matter inhomogeneities as discrete massive particles, we develop the second‐order cosmological perturbation theory. Our approach relies on the weak gravitational field limit. The derived equations for the second‐order scalar, vector, and tensor metric corrections are suitable at arbitrary distances, including regions with nonlinear contrasts of the matter density. We thoroughly verify fulfillment of all Einstein equations, as well as self‐consistency of order assignments. In addition, we achieve logical positive results in the Minkowski background limit. Feasible investigations of the cosmological backreaction manifestations by means of relativistic simulations are also outlined.
E. Canay and M. Eingorn
Physics of the Dark Universe 29 (2020) 100565
DOI: 10.1016/j.dark.2020.100565
https://authors.elsevier.com/a/1aydL7t6qq5DB0
https://arxiv.org/abs/2002.00437
Two distinct perturbative approaches have been recently formulated within General Relativity, arguing for the screening of gravity in the ΛCDM Universe. We compare them and show that the offered screening concepts, each characterized by its own interaction range, can peacefully coexist. Accordingly, we advance a united scheme, determining the gravitational potential at all scales, including regions of nonlinear density contrasts, by means of a simple Helmholtz equation with the effective cosmological screening length. In addition, we claim that cosmic structures may not grow at distances above this Yukawa range and confront its current value with dimensions of the largest known objects in the Universe.
Second-order Cosmological Perturbations Engendered by Point-like MassesMaxim Eingorn
R. Brilenkov and M. Eingorn, Second-order cosmological perturbations engendered by point-like masses, ApJ 845 (2017) 153: http://iopscience.iop.org/article/10.3847/1538-4357/aa81cd
In the ΛCDM framework, presenting nonrelativistic matter inhomogeneities as discrete massive particles, we develop the second‐order cosmological perturbation theory. Our approach relies on the weak gravitational field limit. The derived equations for the second‐order scalar, vector, and tensor metric corrections are suitable at arbitrary distances, including regions with nonlinear contrasts of the matter density. We thoroughly verify fulfillment of all Einstein equations, as well as self‐consistency of order assignments. In addition, we achieve logical positive results in the Minkowski background limit. Feasible investigations of the cosmological backreaction manifestations by means of relativistic simulations are also outlined.
E. Canay and M. Eingorn
Physics of the Dark Universe 29 (2020) 100565
DOI: 10.1016/j.dark.2020.100565
https://authors.elsevier.com/a/1aydL7t6qq5DB0
https://arxiv.org/abs/2002.00437
Two distinct perturbative approaches have been recently formulated within General Relativity, arguing for the screening of gravity in the ΛCDM Universe. We compare them and show that the offered screening concepts, each characterized by its own interaction range, can peacefully coexist. Accordingly, we advance a united scheme, determining the gravitational potential at all scales, including regions of nonlinear density contrasts, by means of a simple Helmholtz equation with the effective cosmological screening length. In addition, we claim that cosmic structures may not grow at distances above this Yukawa range and confront its current value with dimensions of the largest known objects in the Universe.
Microscopic Mechanisms of Superconducting Flux Quantum and Superconducting an...Qiang LI
We have provided microscopic explanations to superconducting flux quantum and (superconducting and normal) persistent current. Flux quantum is generated by current carried by "deep electrons" at surface states. And values of the flux quantum differs according to the electronic states and coupling of the carrier electrons. Generation of persistent carrier electrons does not dissipate energy; instead there would be emission of real phonons and release of corresponding energy into the environment; but the normal carrier electrons involved still dissipate energy. Even for or persistent carriers,there should be a build-up of energy of the middle state and a build-up of the probability of virtual transition of electrons to the middle state, and the corresponding relaxation should exist accordingly.
Solutions of Maxwell Equation for a Lattice System with Meissner EffectQiang LI
We show that Maxwell equation of a lattice system may have Meissner effect solutions when all carriers are surface state electrons. Some limitations on the wave function distributions of electrons in the system are identified.
On Double Elzaki Transform and Double Laplace Transformiosrjce
In this paper, we applied the method double Elzaki transform to solve wave equation in one dimensional and the results are compared with the resultsof double Laplace transform
The Analytical Nature of the Greens Function in the Vicinity of a Simple Poleijtsrd
It is known that the Green function of a boundary value problem is a meromorphic function of a spectral parameter. When the boundary conditions contain integro differential terms, then the meromorphism of the Greens function of such a problem can also be proved. In this case, it is possible to write out the structure of the residue at the singular points of the Greens function of the boundary value problem with integro differential perturbations. An analysis of the structure of the residue allows us to state that the corresponding functions of the original operator are sufficiently smooth functions. Surprisingly, the adjoint operator can have non smooth eigenfunctions. The degree of non smoothness of the eigenfunction of the adjoint operator to an operator with integro differential boundary conditions is clarified. It is indicated that even those conjugations to multipoint boundary value problems have non smooth eigenfunctions. Ghulam Hazrat Aimal Rasa "The Analytical Nature of the Green's Function in the Vicinity of a Simple Pole" Published in International Journal of Trend in Scientific Research and Development (ijtsrd), ISSN: 2456-6470, Volume-4 | Issue-6 , October 2020, URL: https://www.ijtsrd.com/papers/ijtsrd33696.pdf Paper Url: https://www.ijtsrd.com/mathemetics/applied-mathamatics/33696/the-analytical-nature-of-the-greens-function-in-the-vicinity-of-a-simple-pole/ghulam-hazrat-aimal-rasa
Salas, V. (2024) "John of St. Thomas (Poinsot) on the Science of Sacred Theol...Studia Poinsotiana
I Introduction
II Subalternation and Theology
III Theology and Dogmatic Declarations
IV The Mixed Principles of Theology
V Virtual Revelation: The Unity of Theology
VI Theology as a Natural Science
VII Theology’s Certitude
VIII Conclusion
Notes
Bibliography
All the contents are fully attributable to the author, Doctor Victor Salas. Should you wish to get this text republished, get in touch with the author or the editorial committee of the Studia Poinsotiana. Insofar as possible, we will be happy to broker your contact.
Observation of Io’s Resurfacing via Plume Deposition Using Ground-based Adapt...Sérgio Sacani
Since volcanic activity was first discovered on Io from Voyager images in 1979, changes
on Io’s surface have been monitored from both spacecraft and ground-based telescopes.
Here, we present the highest spatial resolution images of Io ever obtained from a groundbased telescope. These images, acquired by the SHARK-VIS instrument on the Large
Binocular Telescope, show evidence of a major resurfacing event on Io’s trailing hemisphere. When compared to the most recent spacecraft images, the SHARK-VIS images
show that a plume deposit from a powerful eruption at Pillan Patera has covered part
of the long-lived Pele plume deposit. Although this type of resurfacing event may be common on Io, few have been detected due to the rarity of spacecraft visits and the previously low spatial resolution available from Earth-based telescopes. The SHARK-VIS instrument ushers in a new era of high resolution imaging of Io’s surface using adaptive
optics at visible wavelengths.
Nutraceutical market, scope and growth: Herbal drug technologyLokesh Patil
As consumer awareness of health and wellness rises, the nutraceutical market—which includes goods like functional meals, drinks, and dietary supplements that provide health advantages beyond basic nutrition—is growing significantly. As healthcare expenses rise, the population ages, and people want natural and preventative health solutions more and more, this industry is increasing quickly. Further driving market expansion are product formulation innovations and the use of cutting-edge technology for customized nutrition. With its worldwide reach, the nutraceutical industry is expected to keep growing and provide significant chances for research and investment in a number of categories, including vitamins, minerals, probiotics, and herbal supplements.
Seminar of U.V. Spectroscopy by SAMIR PANDASAMIR PANDA
Spectroscopy is a branch of science dealing the study of interaction of electromagnetic radiation with matter.
Ultraviolet-visible spectroscopy refers to absorption spectroscopy or reflect spectroscopy in the UV-VIS spectral region.
Ultraviolet-visible spectroscopy is an analytical method that can measure the amount of light received by the analyte.
THE IMPORTANCE OF MARTIAN ATMOSPHERE SAMPLE RETURN.Sérgio Sacani
The return of a sample of near-surface atmosphere from Mars would facilitate answers to several first-order science questions surrounding the formation and evolution of the planet. One of the important aspects of terrestrial planet formation in general is the role that primary atmospheres played in influencing the chemistry and structure of the planets and their antecedents. Studies of the martian atmosphere can be used to investigate the role of a primary atmosphere in its history. Atmosphere samples would also inform our understanding of the near-surface chemistry of the planet, and ultimately the prospects for life. High-precision isotopic analyses of constituent gases are needed to address these questions, requiring that the analyses are made on returned samples rather than in situ.
Toxic effects of heavy metals : Lead and Arsenicsanjana502982
Heavy metals are naturally occuring metallic chemical elements that have relatively high density, and are toxic at even low concentrations. All toxic metals are termed as heavy metals irrespective of their atomic mass and density, eg. arsenic, lead, mercury, cadmium, thallium, chromium, etc.
Earliest Galaxies in the JADES Origins Field: Luminosity Function and Cosmic ...Sérgio Sacani
We characterize the earliest galaxy population in the JADES Origins Field (JOF), the deepest
imaging field observed with JWST. We make use of the ancillary Hubble optical images (5 filters
spanning 0.4−0.9µm) and novel JWST images with 14 filters spanning 0.8−5µm, including 7 mediumband filters, and reaching total exposure times of up to 46 hours per filter. We combine all our data
at > 2.3µm to construct an ultradeep image, reaching as deep as ≈ 31.4 AB mag in the stack and
30.3-31.0 AB mag (5σ, r = 0.1” circular aperture) in individual filters. We measure photometric
redshifts and use robust selection criteria to identify a sample of eight galaxy candidates at redshifts
z = 11.5 − 15. These objects show compact half-light radii of R1/2 ∼ 50 − 200pc, stellar masses of
M⋆ ∼ 107−108M⊙, and star-formation rates of SFR ∼ 0.1−1 M⊙ yr−1
. Our search finds no candidates
at 15 < z < 20, placing upper limits at these redshifts. We develop a forward modeling approach to
infer the properties of the evolving luminosity function without binning in redshift or luminosity that
marginalizes over the photometric redshift uncertainty of our candidate galaxies and incorporates the
impact of non-detections. We find a z = 12 luminosity function in good agreement with prior results,
and that the luminosity function normalization and UV luminosity density decline by a factor of ∼ 2.5
from z = 12 to z = 14. We discuss the possible implications of our results in the context of theoretical
models for evolution of the dark matter halo mass function.
1. Sweeping Discussions On Dirac Fields
Roa, F. J. P.
We write
(1)
tni
LL
ffe LLL ),()()( 2122 ψψψψ +=
as a Lagrangian for a basic electron theory that can be outlined from an SU(2)XU(1)
construction that excludes as yet the additional fermions needed in the full electroweak
theory. Lagrangian (1) includes an effective Lagrangian ffeL )( 2ψ for the electron 2ψ
and an interaction Lagrangian tni
LL
L ),( 21 ψψ exclusive only for the lefthanded
(electron) neutrino L
1ψ , which is massless, and the lefthanded electron L
2ψ that has mass.
The effective Lagrangian (for the electron 2ψ ), aside from the free Lagrangian 02 )(ψL
present in it, also contains tniL )( 2ψ , which serves as an interaction Lagrangian in the
said effective lagrangian ( ffeL )( 2ψ ) that includes the interactions of the electron with
the Higgs boson η , the electromagnetic field me
Aµ that is massless, and one massive field
µZ .
(2.1)
tniffe LLL )()()( 2022 ψψψ +=
(2.2)
( )
( )LRR
RLL
mi
mi
miL
222
222
222202 )(
ψψγψ
ψψγψ
ψψψγψψ
ψµ
µ
ψµ
µ
ψµ
µ
−∂
+−∂=
=−∂=
Let it be noted that all equations appearing in this document are in Heaviside units in
which 1== ch and that the Dirac mass ψm is simply given in terms of the Yukawa
coupling constant y and the non-zero vacuum expectation value (vev) β of the Higgs
field,
2. (2.3)
βψ ym =
(2.4)
( ) 22222 tan)( ψαγψψψηψ µµ
µ
ZeAeyL me
tni ++−=
This Lagrangian can ofcourse be viewed in terms of the lefthanded electron and its
counter-part, R
2ψ .
(2.5.1)
( ) 2
5
2 1
2
1
ψγψ +=L
(2.5.2)
( ) 2
5
2 1
2
1
ψγψ −=R
(I must emphasize that in this document, our definitions for L
2ψ and R
2ψ are as given by
the preceding equations above.)
Given (2.5.1) and (2.5.2), the said effective Lagrangian can be decomposed under the
following expressions
(2.6.1)
222222 ψψψψψψ =+ RLLR
(2.6.2)
222222 ψγψψγψψγψ µµµ
=+ RRLL
(2.6.3)
222222 ψγψψγψψγψ µ
µ
µ
µ
µ
µ
∂=∂+∂ RRLL
For the interaction Lagrangian tni
LL
L ),( 21 ψψ , one thing to notice in this is that this
excludes the righthanded electron and represents the interactions of the massless
lefthanded neutrino L
1ψ and lefthanded electron with the weak gauge bosons.
(2.7)
3. ( ))(
12
)(
21
1
22
1
21
)sin2(
)cossin2(),(
+−−
−
+
−−=
µ
µ
µ
µ
µ
µ
ψγψψγψα
ψγψααψψ
WWe
ZeL
LLLL
LL
tni
LL
Let us take ffeL )( 2ψ from (1) and with it form the action
(3.1)
ffeffe LxdS )()( 2
4
2 ψψ ∫=
We may think of it as an effective electron theory that we can outline from a basic
SU(2)XU(1) construction without as yet the additional fermions of electroweak theory.
In the said action (3.1), we may proceed with the four integral contained in it
(3.2)
∫ ∑∫
∂+∂=∂
=
3
1
220
0
2
30
22
4
l
l
l
ixdxdixd ψγψγψψγψ µ
µ r
From (3.2), say we perform the one integral over time ( tx =0
) first, assuming we are
given with two end-points ( 00
BA xandx ) in time and thus, by integration by-parts we
have
(3.3)
[ ] ∫∫ ∂−=∂ 2
0
20
0
)(
)(
2
0
220
0
2
0
)(
0
0
ψγψψγψψγψ ixdiixd
Bx
Ax
We can use this to write one four integral in (3.2) as
(3.4)
[ ] ∫∫ ∫ ∂−=∂ 2
0
20
4
)(
)(
2
0
2020
0
2
4
)(
0
0
ψγψψγψσψγψ ixdidixd
Bx
Ax
where for example, 0
σd is a short for
(3.5)
32130
dxdxdxxdd ==
r
σ
In the same way we can manipulate for any given space part in (3.2)
(3.6)
4. [ ] ∫∫ ∫ ∂−=∂ 22
4
)(
)(
2222
4
)( ψγψψγψσψγψ l
l
Bx
Ax
l
ll
l
ixdidixd
l
l
Thus, by integration by-parts we are able to re-write (3.2) into a desired form
(3.7)
[ ] ∫∫ ∫ ∂−=∂ 22
4
)(
)(
2222
4
)( ψγψψγψσψγψ µ
µ
µ
µµ
µ µ
µ
ixdidixd
Bx
Ax
Consequently, using (3.7) we may put (3.1) in the following form
(3.8.1)
[ ] ( )∫∫ ++∂−= 222222
4)(
)(222 )()( ψψψψβψγψψγψσψ µ
µ
µ
µ
µ
µ q
Bx
Axffe FyixdidS
(3.8.2)
µ
µ
µ
µ
αγγη ZeeAyF me
q tan−−=
What we have done here in using integration by-parts (3.7) in (3.1) is a recasting of this
action, which is held as an effective action for the spinor field 2ψ , into an action
ffeS )( 2ψ for the adjoint spinor field 2ψ .
(3.9)
( )∫
∫
++∂−=
==
222222
4
2
4
2
)(
)()(
ψψψψβψγψ
ψψ
µ
µ q
ffeffe
Fyixd
LxdS
We may think of (3.1) and (3.9) as two separate theories that are adjoint to each other. In
these actions, we can take 2ψ and 2ψ as two independent spinor fields and we can obtain
the total simultaneous variations of these actions in terms of the variations of the cited
field variables.
From (3.1) we obtain the total variation
(3.10.1)
[ ]
( )
( ) 2222
4
2222
4
)(
)(222
)(
)(
δψψψβγψ
ψψβψγψδ
δψγψσψδ
µ
µ
µ
µ
µ
µ
µ
µ
∫
∫
∫
++∂
−−−∂
+=
q
q
Bx
Ax
Fyixd
Fyixd
idS
5. while from (3.9) we have
(3.10.2)
[ ]
( )
( ) 2222
4
2222
4
)(
)(222
)(
)(
δψψψβγψ
ψψβψγψδ
ψγψδσψδ
µ
µ
µ
µ
µ
µ
µ
µ
∫
∫
∫
++∂
−−−∂
+−=
q
q
Bx
Ax
Fyixd
Fyixd
idS
In the classical context, we can impose the boundary condition that the varied fields
( 2δψ and 2ψδ ) vanish at the two end-points A and B. Thus, rendering the effective
forms of (3.10.1) and (3.10.2) equivalent
(3.11)
ffeffe SS )()( 22 ψδψδ =
To get Dirac’s first order equation of motion for the independent field 2ψ , we vary
action (3.1) with respect to the adjoint spinor 2ψ alone and this yields
(4.1)
)(
)(
2
2
2
2
2
2
2
2
4
22
)(
)()(
)/(
Bx
Ax
ffe
ffeffe
L
d
LL
xdS
µ
µ
ψδ
ψδ
ψδσ
ψδ
ψδ
ψδ
ψδ
ψδψδψδ
µ
µ
µ
µ
∂
+
∂
∂−=
∫
∫
This, obtained by invoking the commutativity in
(4.2)
δδ µµ ∂=∂
and after integration by-parts. Again, in the classical context we impose the spacetime
boundary condition on the varied field 2ψδ to obtain the effective form of (4.1)
6. (4.3.1)
∫
∂
∂−=
2
2
2
2
2
4
22
)()(
)/(
ψδ
ψδ
ψδ
ψδ
ψδψδψδ
µ
µ
ffeffe
ffe
LL
xdS
(4.3.2)
0)()( 22 == BA ψδψδ
Also, in the classical context, we render this effective variation stationary
(4.4.1)
0)/( 22 =ffeS ψδψδ
we obtain the Euler-Lagrange equation
(4.4.2)
0
)()(
2
2
2
2
=
∂
∂−
ψδ
ψδ
ψδ
ψδ
µ
µ
ffeffe LL
and upon noting that
(4.4.3)
0
)(
2
2
=
∂ ψδ
ψδ
µ
ffeL
and
(4.4.4)
222
2
2 )(
ψψβψγ
ψδ
ψδ
µ
µ
q
ffe
Fyi
L
−−∂=
we arrive at the said first order equation
(4.4.5)
0222 =−−∂ ψψβψγ µ
µ
qFyi
7. Ref’s:
[1]W. Hollik, Quantum field theory and the Standard Model, arXiv:1012.3883v1 [hep-
ph]
[2]Baal, P., A COURSE IN FIELD THEORY,
http://www.lorentz.leidenuniv.nl/~vanbaal/FTcourse.html
[3]’t Hooft, G., THE CONCEPTUAL BASIS OF QUANTUM FIELD THEORY,
http://www.phys.uu.nl/~thooft/
[4]Siegel, W., FIELDS, arXiv:hep-th/9912205 v2
[5]Wells, J. D., Lectures on Higgs Boson Physics in the Standard Model and Beyond,
arXiv:0909.4541v1
[6]Cardy, J., Introduction to Quantum Field Theory
[7]Gaberdiel, M., Gehrmann-De Ridder, A., Quantum Field Theory