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Paul Giem on The Natural Limits of Neo-Darwinian Evolution 9-29-2012 13th in a series on the book " In the Beginning: Science and Scripture Confirm Creation " (edited by Bryan W. Ball).  This chapter (by John C. Walton) discusses Darwinism as a big theory in the tradition of gravity, electromagnetic theory, and atomic theory that, like them, needs qualification.  He discusses the scientific weaknesses of evolution as a prediction-making theory, using the examples of junk DNA, the tree of life, and gradualism, concluding that the theory should be downsized. http://www.adventistbookcenter.com/Detail.tpl?sku=0816326150 http://www.adventistbookcenter.com/Product_Info/Chapters/0816326150.pdf For additional recordings on various topics regarding faith and science visit: ItsAboutGod.tv/sls

"The Limits of Organic Evolution" is an article from The American Naturalist, Volume 20 . View more articles from The American Naturalist . View this article on JSTOR . View this article's JSTOR metadata . You may also retrieve all of this items metadata in JSON at the following URL: https://archive.org/metadata/jstor-2450339

The causal limit usually considered in cosmology is the particle horizon, delimiting the possibilities of causal connection in the expanding universe. However it is not a realistic indicator of the effective local limits of important interactions in spacetime. We consider here the matter horizon for the Solar System, that is,the comoving region which has contributed matter to our local physical environment. This lies inside the effective domain of dependence, which (assuming the universe is dominated by dark matter along with baryonic matter and vacuum-energy-like dark energy) consists of those regions that have had a significant active physical influence on this environment through effects such as matter accretion and acoustic waves. It is not determined by the velocity of light c, but by the flow of matter perturbations along their world lines and associated gravitational effects. We emphasize how small a region the perturbations which became our Galaxy occupied, relative to the observable universe -- even relative to the smallest-scale perturbations detectable in the cosmic microwave background radiation. Finally, looking to the future of our cosmic domain, we suggest simple dynamical criteria for determining the present domain of influence and the future matter horizon. The former is the radial distance at which our local region is just now separating from the cosmic expansion. The latter represents the limits of growth of the matter horizon in the far future.

The causal limit usually considered in cosmology is the particle horizon, delimiting the possibilities of causal connection in the expanding universe. However it is not a realistic indicator of the effective local limits of important interactions in spacetime. We consider here the matter horizon for the Solar System, that is,the comoving region which has contributed matter to our local physical environment. This lies inside the effective domain of dependence, which (assuming the universe is dominated by dark matter along with baryonic matter and vacuum-energy-like dark energy) consists of those regions that have had a significant active physical influence on this environment through effects such as matter accretion and acoustic waves. It is not determined by the velocity of light c, but by the flow of matter perturbations along their world lines and associated gravitational effects. We emphasize how small a region the perturbations which became our Galaxy occupied, relative to the observable universe -- even relative to the smallest-scale perturbations detectable in the cosmic microwave background radiation. Finally, looking to the future of our cosmic domain, we suggest simple dynamical criteria for determining the present domain of influence and the future matter horizon. The former is the radial distance at which our local region is just now separating from the cosmic expansion. The latter represents the limits of growth of the matter horizon in the far future.

The causal limit usually considered in cosmology is the particle horizon, delimiting the possibilities of causal connection in the expanding universe. However it is not a realistic indicator of the effective local limits of important interactions in spacetime. We consider here the matter horizon for the Solar System, that is,the comoving region which has contributed matter to our local physical environment. This lies inside the effective domain of dependence, which (assuming the universe is dominated by dark matter along with baryonic matter and vacuum-energy-like dark energy) consists of those regions that have had a significant active physical influence on this environment through effects such as matter accretion and acoustic waves. It is not determined by the velocity of light c, but by the flow of matter perturbations along their world lines and associated gravitational effects. We emphasize how small a region the perturbations which became our Galaxy occupied, relative to the observable universe -- even relative to the smallest-scale perturbations detectable in the cosmic microwave background radiation. Finally, looking to the future of our cosmic domain, we suggest simple dynamical criteria for determining the present domain of influence and the future matter horizon. The former is the radial distance at which our local region is just now separating from the cosmic expansion. The latter represents the limits of growth of the matter horizon in the far future.

It is tempting to treat frequency trends from the Google Books data sets as indicators of the "true" popularity of various words and phrases. Doing so allows us to draw quantitatively strong conclusions about the evolution of cultural perception of a given topic, such as time or gender. However, the Google Books corpus suffers from a number of limitations which make it an obscure mask of cultural popularity. A primary issue is that the corpus is in effect a library, containing one of each book. A single, prolific author is thereby able to noticeably insert new phrases into the Google Books lexicon, whether the author is widely read or not. With this understood, the Google Books corpus remains an important data set to be considered more lexicon-like than text-like. Here, we show that a distinct problematic feature arises from the inclusion of scientific texts, which have become an increasingly substantive portion of the corpus throughout the 1900s. The result is a surge of phrases typical to academic articles but less common in general, such as references to time in the form of citations. We highlight these dynamics by examining and comparing major contributions to the statistical divergence of English data sets between decades in the period 1800--2000. We find that only the English Fiction data set from the second version of the corpus is not heavily affected by professional texts, in clear contrast to the first version of the fiction data set and both unfiltered English data sets. Our findings emphasize the need to fully characterize the dynamics of the Google Books corpus before using these data sets to draw broad conclusions about cultural and linguistic evolution.

IX, 347 p. ; 21 cm

Explore AI podcasters testing historical TTS milestones in real-time. From ELIZA to AudioLM, they showcase tech evolution, critique each other, and analyze results in this groundbreaking existential challenge."

This paper reports on some new inequalities of Margolus-Levitin-Mandelstam-Tamm-type involving the speed of quantum evolution between two orthogonal pure states. The clear determinant of the qualitative behavior of this time scale is the statistics of the energy spectrum. An often-overlooked correspondence between the real-time behavior of a quantum system and the statistical mechanics of a transformed (imaginary-time) thermodynamic system appears promising as a source of qualitative insights into the quantum dynamics.

This paper reports on some new inequalities of Margolus-Levitin-Mandelstam-Tamm-type involving the speed of quantum evolution between two orthogonal pure states. The clear determinant of the qualitative behavior of this time scale is the statistics of the energy spectrum. An often-overlooked correspondence between the real-time behavior of a quantum system and the statistical mechanics of a transformed (imaginary-time) thermodynamic system appears promising as a source of qualitative insights into the quantum dynamics.

Book digitized by Google from the library of Harvard University and uploaded to the Internet Archive by user tpb.

This paper is in the public domain in USA. Metadata comes from the CrossRef API, see full record in the source URL below.

Evolution of the Voyager 1 and 2 Space Probes. Hydrogen without limits + artificial intelligence. Evoluciòn de las Sondas Espaciales Voyager 1 y 2.  Hidrògeno sin limites + inteligencia artificial. El hidrógeno es el elemento químico más abundante del universo, representando alrededor del 75% de la materia visible:  Es el primer elemento que se formó después del Big Bang.  En el espacio interestelar, el hidrógeno se encuentra junto con polvo y moléculas complejas en estado gaseoso, como el agua, el amoníaco y el metanol. Se encuentra en las estrellas y en los planetas gaseosos.  Es el combustible principal de las estrellas, donde se fusiona para producir energía y helio.  En la Tierra, el hidrógeno está combinado con otros elementos, como el oxígeno y el carbono, formando agua y compuestos orgánicos.  El hidrógeno se encuentra en el universo en forma atómica y en estado de plasma: En estado de plasma, el hidrógeno tiene una alta conductividad eléctrica y es el origen de la luz emitida por las estrellas. Bajo condiciones normales de presión y temperatura, el hidrógeno existe como gas diatómico, H2.  El hidrógeno es un elemento importante para estudiar el universo y su formación estelar: Se puede observar cómo se mueven las estrellas y el gas en las galaxias. Se puede detectar el estado del hidrógeno neutro en la época previa a la formación de las primeras estrellas. Dedicado a Aurora Lucia Cabral y a V'ger. .......

Evolution of the Voyager 1 and 2 Space Probes. Hydrogen without limits + artificial intelligence. Evoluciòn de las Sondas Espaciales Voyager 1 y 2.  Hidrògeno sin limites + inteligencia artificial. El hidrógeno es el elemento químico más abundante del universo, representando alrededor del 75% de la materia visible:  Es el primer elemento que se formó después del Big Bang.  En el espacio interestelar, el hidrógeno se encuentra junto con polvo y moléculas complejas en estado gaseoso, como el agua, el amoníaco y el metanol. Se encuentra en las estrellas y en los planetas gaseosos.  Es el combustible principal de las estrellas, donde se fusiona para producir energía y helio.  En la Tierra, el hidrógeno está combinado con otros elementos, como el oxígeno y el carbono, formando agua y compuestos orgánicos.  El hidrógeno se encuentra en el universo en forma atómica y en estado de plasma: En estado de plasma, el hidrógeno tiene una alta conductividad eléctrica y es el origen de la luz emitida por las estrellas. Bajo condiciones normales de presión y temperatura, el hidrógeno existe como gas diatómico, H2.  El hidrógeno es un elemento importante para estudiar el universo y su formación estelar: Se puede observar cómo se mueven las estrellas y el gas en las galaxias. Se puede detectar el estado del hidrógeno neutro en la época previa a la formación de las primeras estrellas. Dedicado a Aurora Lucia Cabral y a V'ger. .......

Book digitized by Google from the library of Harvard University and uploaded to the Internet Archive by user tpb.

Book digitized by Google from the library of the University of Michigan and uploaded to the Internet Archive by user tpb.

Book digitized by Google from the library of the University of Michigan and uploaded to the Internet Archive by user tpb.

Philosophy has long been a field that thrives on paradoxes, contradictions, and the perpetual reinvention of ideas. Let us shortly explore the limits of philosophical thought through the lens of neutrosophy, by challenging traditional dichotomies such as tautology vs. nihilism and thesis vs. antithesis. That is what neutrosophy seeks to do: introduce a pluralistic and process-oriented approach to philosophical inquiry.

Philosophy has long been a field that thrives on paradoxes, contradictions, and the perpetual reinvention of ideas. Let us shortly explore the limits of philosophical thought through the lens of neutrosophy, by challenging traditional dichotomies such as tautology vs. nihilism and thesis vs. antithesis. That is what neutrosophy seeks to do: introduce a pluralistic and process-oriented approach to philosophical inquiry.

Includes bibliographical references (p. 277-305) and index

We report infrared spectroscopic observations of HD 105, a nearby ($\sim 40$ pc) and relatively young ($\sim 30$ Myr) G0 star with excess infrared continuum emission, which has been modeled as arising from an optically thin circumstellar dust disk with an inner hole of size $\gtrsim 13$ AU. We have used the high spectral resolution mode of the Infrared Spectrometer (IRS) on the Spitzer Space Telescope to search for gas emission lines from the disk. The observations reported here provide upper limits to the fluxes of H$_2$ S(0) 28$\mu$m, H$_2$ S(1) 17$\mu$m, H$_2$ S(2) 12 $\mu$m, [FeII] 26$\mu$m, [SiII] 35$\mu$m, and [SI] 25$\mu$m infrared emission lines. The H$_2$ line upper limits directly place constraints on the mass of warm molecular gas in the disk: $M({\rm H_2}) < 4.6$, 3.8$\times 10^{-2}$, and $3.0\times 10^{-3}$ M$_J$ at $T= 50$, 100, and 200 K, respectively. We also compare the line flux upper limits to predictions from detailed thermal/chemical models of various gas distributions in the disk. These comparisons indicate that if the gas distribution has an inner hole with radius $r_{i,gas}$, the surface density at that inner radius is limited to values ranging from $\lesssim 3$ gm cm$^{-2}$ at $r_{i,gas}=0.5$ AU to 0.1 gm cm$^{-2}$ at $r_{i,gas}= 5-20$ AU. These values are considerably below the value for a minimum mass solar nebula, and suggest that less than 1 M$_J$ of gas (at any temperature) exists in the 1-40 AU planet-forming region. Therefore, it is unlikely that there is sufficient gas for gas giant planet formation to occur in HD 105 at this time.

We report infrared spectroscopic observations of HD 105, a nearby ($\sim 40$ pc) and relatively young ($\sim 30$ Myr) G0 star with excess infrared continuum emission, which has been modeled as arising from an optically thin circumstellar dust disk with an inner hole of size $\gtrsim 13$ AU. We have used the high spectral resolution mode of the Infrared Spectrometer (IRS) on the Spitzer Space Telescope to search for gas emission lines from the disk. The observations reported here provide upper limits to the fluxes of H$_2$ S(0) 28$\mu$m, H$_2$ S(1) 17$\mu$m, H$_2$ S(2) 12 $\mu$m, [FeII] 26$\mu$m, [SiII] 35$\mu$m, and [SI] 25$\mu$m infrared emission lines. The H$_2$ line upper limits directly place constraints on the mass of warm molecular gas in the disk: $M({\rm H_2}) < 4.6$, 3.8$\times 10^{-2}$, and $3.0\times 10^{-3}$ M$_J$ at $T= 50$, 100, and 200 K, respectively. We also compare the line flux upper limits to predictions from detailed thermal/chemical models of various gas distributions in the disk. These comparisons indicate that if the gas distribution has an inner hole with radius $r_{i,gas}$, the surface density at that inner radius is limited to values ranging from $\lesssim 3$ gm cm$^{-2}$ at $r_{i,gas}=0.5$ AU to 0.1 gm cm$^{-2}$ at $r_{i,gas}= 5-20$ AU. These values are considerably below the value for a minimum mass solar nebula, and suggest that less than 1 M$_J$ of gas (at any temperature) exists in the 1-40 AU planet-forming region. Therefore, it is unlikely that there is sufficient gas for gas giant planet formation to occur in HD 105 at this time.

We report infrared spectroscopic observations of HD 105, a nearby ($\sim 40$ pc) and relatively young ($\sim 30$ Myr) G0 star with excess infrared continuum emission, which has been modeled as arising from an optically thin circumstellar dust disk with an inner hole of size $\gtrsim 13$ AU. We have used the high spectral resolution mode of the Infrared Spectrometer (IRS) on the Spitzer Space Telescope to search for gas emission lines from the disk. The observations reported here provide upper limits to the fluxes of H$_2$ S(0) 28$\mu$m, H$_2$ S(1) 17$\mu$m, H$_2$ S(2) 12 $\mu$m, [FeII] 26$\mu$m, [SiII] 35$\mu$m, and [SI] 25$\mu$m infrared emission lines. The H$_2$ line upper limits directly place constraints on the mass of warm molecular gas in the disk: $M({\rm H_2}) < 4.6$, 3.8$\times 10^{-2}$, and $3.0\times 10^{-3}$ M$_J$ at $T= 50$, 100, and 200 K, respectively. We also compare the line flux upper limits to predictions from detailed thermal/chemical models of various gas distributions in the disk. These comparisons indicate that if the gas distribution has an inner hole with radius $r_{i,gas}$, the surface density at that inner radius is limited to values ranging from $\lesssim 3$ gm cm$^{-2}$ at $r_{i,gas}=0.5$ AU to 0.1 gm cm$^{-2}$ at $r_{i,gas}= 5-20$ AU. These values are considerably below the value for a minimum mass solar nebula, and suggest that less than 1 M$_J$ of gas (at any temperature) exists in the 1-40 AU planet-forming region. Therefore, it is unlikely that there is sufficient gas for gas giant planet formation to occur in HD 105 at this time.

Limits are imposed upon the possible rate of change of extra spatial dimensions in a decrumpling model Universe with time variable spatial dimensions (TVSD) by considering the time variation of (1+3)-dimensional Newton's constant. Previous studies on the time variation of (1+3)-dimensional Newton's constant in TVSD theory had not been included the effects of the volume of the extra dimensions and the effects of the surface area of the unit sphere in D-space dimensions. Our main result is that the absolute value of the present rate of change of spatial dimensions to be less than about 10^{-14}yr^{-1}. Our results would appear to provide a prima facie case for ruling the TVSD model out. We show that based on observational bounds on the present-day variation of Newton's constant, one would have to conclude that the spatial dimension of the Universe when the Universe was at the Planck scale to be less than or equal to 3.09. If the dimension of space when the Universe was at the Planck scale is constrained to be fractional and very close to 3, then the whole edifice of TVSD model loses credibility.

The Sturm-Liouville hierarchy of evolution equations was introduced in [Adv. Nonlinear Stud. 11 (2011), 555-591] and includes the Korteweg-de Vries and the Camassa-Holm hierarchies. We discuss some solutions of this hierarchy which are obtained as limits of algebro-geometric solutions. The initial data of our solutions are (generalized) reflectionless Sturm-Liouville potentials [Stoch. Dyn. 8 (2008), 413-449].

We use gravitational lenses from the Cosmic Lens All-Sky Survey (CLASS) to constrain the evolution of galaxies since redshift $z \sim 1$ in the current $\LCDM$ cosmology. This constraint is unique as it is based on a mass-selected lens sample of galaxies. Our method of statistical analysis is the same as in Chae (2003). We parametrise the early-type number density evolution in the form of $(1+z)^{\nu_n}$ and the velocity dispersion as $(1+z)^{\nu_v}$. We find that $\nu_n=-0.11^{+0.82}_{-0.89}$ ($1\sigma$) if we assume $\nu_v =0$, implying that the number density of early-type galaxies is within 50% to 164% of the present-day value at redshift $z=1$. Allowing the velocity dispersion to evolve, we find that $\nu_v=-0.4^{+0.5}_{-0.4}$ ($1\sigma$), indicating that the velocity dispersion must be within 57% and 107% of the present-day value at $z=1$. These results are consistent with the early formation and passive evolution of early-type galaxies. More stringent limits from lensing can be obtained from future large lens surveys and by using very high-redshift quasars ($z \ga 5$) such as those found from the Sloan Digital Sky Survey.

We have carried out a sensitive search for gas emission lines at infrared and millimeter wavelengths for a sample of 15 young sun-like stars selected from our dust disk survey with the Spitzer Space Telescope. We have used mid-infrared lines to trace the warm (300-100 K) gas in the inner disk and millimeter transitions of 12CO to probe the cold (~20 K) outer disk. We report no gas line detections from our sample. Line flux upper limits are first converted to warm and cold gas mass limits using simple approximations allowing a direct comparison with values from the literature. We also present results from more sophisticated models following Gorti and Hollenbach (2004) which confirm and extend our simple analysis. These models show that the SI line at 25.23 micron can set constraining limits on the gas surface density at the disk inner radius and traces disk regions up to a few AU. We find that none of the 15 systems have more than 0.04 MJ of gas within a few AU from the disk inner radius for disk radii from 1 AU up to ~40 AU. These gas mass upper limits even in the 8 systems younger than ~30 Myr suggest that most of the gas is dispersed early. The gas mass upper limits in the 10-40 AU region, that is mainly traced by our CO data, are

The James Webb Space Telescope (JWST) is expected to revolutionize our understanding of the high-redshift Universe, and may be able to test the prediction that the first, chemically pristine (population III) stars formed with very high characteristic masses. Since isolated population III stars are likely to be beyond the reach of JWST, small population III galaxies may offer the best prospects of directly probing the properties of metal-free stars. Here, we present Yggdrasil, a new spectral synthesis code geared towards the first galaxies. Using this model, we explore the JWST imaging detection limits for population III galaxies and investigate to what extent such objects may be identified based on their JWST colours. We predict that JWST should be able to detect population III galaxies with stellar population masses as low as ~10^5 Msolar at z=10 in ultra deep exposures. Over limited redshift intervals, it may also be possible to use colour criteria to select population III galaxy candidates for follow-up spectroscopy. The colours of young population III galaxies dominated by direct star light can be used to probe the stellar initial mass function (IMF), but this requires almost complete leakage of ionizing photons into the intergalactic medium. The colours of objects dominated by nebular emission show no corresponding IMF sensitivity. We also note that a clean selection of population III galaxies at z~7-8 can be achieved by adding two JWST/MIRI filters to the JWST/NIRCam filter sets usually discussed in the context of JWST ultra deep fields.

We explore when supernovae can (and cannot) regulate the star formation and bulge growth in galaxies based on a sample of 18 simulated galaxies. The simulations include key physics such as evaporation and conduction, neglected in prior work, and required to correctly model superbubbles resulting from stellar feedback. We show that for galaxies with virial masses $>10^{12}\;M_\odot$, supernovae alone cannot prevent excessive star formation. This failure occurs due to a shutdown of galactic winds, with wind mass loadings falling from $\eta\sim10$ to $\eta

We explore when supernovae can (and cannot) regulate the star formation and bulge growth in galaxies based on a sample of 18 simulated galaxies. The simulations include key physics such as evaporation and conduction, neglected in prior work, and required to correctly model superbubbles resulting from stellar feedback. We show that for galaxies with virial masses $>10^{12}\;M_\odot$, supernovae alone cannot prevent excessive star formation. This failure occurs due to a shutdown of galactic winds, with wind mass loadings falling from $\eta\sim10$ to $\eta

We explore when supernovae can (and cannot) regulate the star formation and bulge growth in galaxies based on a sample of 18 simulated galaxies. The simulations include key physics such as evaporation and conduction, neglected in prior work, and required to correctly model superbubbles resulting from stellar feedback. We show that for galaxies with virial masses $>10^{12}\;M_\odot$, supernovae alone cannot prevent excessive star formation. This failure occurs due to a shutdown of galactic winds, with wind mass loadings falling from $\eta\sim10$ to $\eta