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Although an application of the approach presented here would likely be feasible with current experiments only for very optimistic dark matter scenarios, the improved sensitivity of upcoming experiments could enable this technique to be used to study a wider range of dark matter models.
This sheds some optimistic prospects for the otherwise dire experimental and observational outlook of detecting dark matter produced by freeze-in.

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Role of volume in gas law?
5 answers
Volume plays a crucial role in various gas laws and their applications. In the context of star formation laws, volume densities of gas (HI+H2) in galaxies exhibit a tight correlation with the star formation rate (SFR), emphasizing the importance of considering three-dimensional density profiles by accounting for the radial growth of gaseous discs. Additionally, in the study of heat radiation from gas volumes, the laws of radiation from gas volumes have been shown to impact fuel saving and environmental pressure reduction by considering the dimensions, power, and geometrical position of radiative gas volumes, highlighting the significance of volume in heat transfer calculations. Therefore, understanding and incorporating volume measurements are essential in various fields to comprehend and predict the behavior of gases accurately.
How do galaxy clusters contribute to the large-scale structure of the universe?
5 answers
Galaxy clusters play a crucial role in shaping the large-scale structure of the universe through various mechanisms. The growth of the most massive halos via accretion and mergers generates shocks, bulk motions, and turbulence, injecting kinetic energy that contributes to heating and virialization, impacting the intra-cluster medium. Additionally, the expansion of the universe, incorporating a cosmological constant, affects the formation of large-scale structures, leading to gravitational phase transitions and cosmic energy equations within the system of galaxies. Observations of extragalactic filaments and the mapping of large-scale density fluctuations using statistical parameters like power spectra provide insights into the structure of the universe and constrain models of dark matter, dark energy, inflation, and brane cosmology. Tools like CLASS-PT and theoretical error likelihood approaches enable precise cosmological analyses of galaxy clustering data, extracting valuable cosmological information.
What does the Cheshire Cat represent in Alice's unconsciousness as a feeling or emotion?
5 answers
The Cheshire Cat in Lewis Carroll's "Alice's Adventures in Wonderland" symbolizes various concepts across different contexts. In the context of modern normative decision theory, the Cheshire Cat provides clear and simple advice, highlighting significant tenets often overlooked in engineering design. Additionally, the quantum Cheshire cat effect, inspired by the dis-embodied grin of the Cheshire Cat, is a phenomenon in quantum theory where a particle's properties can be separated from its location through weak probing, as demonstrated with photons and neutrons in experiments. Furthermore, in a creative context, the Cheshire Cat metaphorically represents 'madness' and the dominance of the unconscious in the artistic process, as articulated by Lewis Carroll, influencing the works of various artists. Thus, the Cheshire Cat embodies advice, quantum phenomena, and artistic inspiration, reflecting a multifaceted symbol in different realms.
What is the small things to study the universe ?
4 answers
Studying the universe involves investigating a wide range of celestial objects and phenomena, from dwarf irregular galaxies to ultrafaint dwarf galaxies, cosmic expansion, and even the distribution of dark matter using strongly lensed systems. Dwarf irregular galaxies provide insights into total matter distribution, while ultrafaint dwarf galaxies offer a glimpse into early galaxy formation. Cosmic expansion, likened to a balloon's surface expanding, is a fundamental concept explored theoretically and experimentally. Additionally, the distribution of dark matter on small scales can be probed through the unique anisotropic signature in the lensing deflection field due to line-of-sight halos. These small-scale studies contribute significantly to our understanding of the universe's dynamics, evolution, and composition.
What are the current technological limitations and future prospects for developing and deploying Dyson spheres on a large scale?
4 answers
yson Spheres, envisioned as megastructures surrounding stars to harness their energy, face current technological constraints and future potential. Presently, Dyson Swarms are favored over solid Dyson Spheres for efficiency. Studies set stringent upper limits on partially completed Dyson Spheres in the Milky Way, emphasizing challenges in detecting them due to natural sources of infrared radiation. Exploring Dyson Spheres around black holes, it is found that harnessing energy from accretion discs could sustain advanced civilizations, with detectability through waste heat radiation across various wavelengths. Additionally, techniques combining Gaia data with ground-based surveys offer a complementary approach to identify Dyson Spheres based on distance discrepancies, hinting at potential historians. Spect. re shiftingay. Spect. . . . . . Som of of
What are some limitations and challenges of using deep learning models for growth ring boundary detection?
4 answers
Using deep learning models for growth ring boundary detection faces limitations and challenges. For instance, in the context of camouflaged object detection, existing deep-learning methods struggle with accurately identifying objects with fine structures. Similarly, in the study of ring galaxies, current catalogs are limited due to the time-consuming manual analysis required to accumulate a substantial sample of rings, hindering further research into their properties. Moreover, the detection of tree rings is a challenging task, as manual evaluation typically involves physical devices and is labor-intensive, prompting the development of neural network-based solutions for automated detection and analysis. These challenges highlight the need for more advanced deep learning approaches to improve the accuracy and efficiency of growth ring boundary detection.
Is there geometrical beaming in ultraluminous x-ray sources?
4 answers
Geometrical beaming in ultraluminous X-ray sources (ULXs) remains a topic of investigation with varying conclusions. Studies suggest that the hard X-rays in ULXs may not be significantly beamed towards the symmetric axis, as indicated by the limited fraction of hard X-rays reprocessed on the outer disk in some ULX systems. Conversely, observations of ULX NGC~300 ULX-1 imply minimal geometric beaming effects, supporting the notion that it is powered by accretion onto a neutron star rather than intense beaming. Additionally, the analysis of ULXs NGC5408 X-1, NGC6946 X-1, M82 X-1, NGC1313 X-1, and IC342 X-1 suggests that the maximum X-ray luminosity in ULXs may primarily depend on the black hole mass rather than geometrical beaming effects.
Dark photons and dark neutrinos are the same or sterile neutrinos?
5 answers
Dark photons and dark neutrinos are distinct entities. Dark photons are hypothetical particles associated with dark matter interactions, while sterile neutrinos are neutrino variants that do not participate in weak interactions. Sterile neutrinos can be involved in dark matter scenarios, acting as mediators between dark matter and the Standard Model sector. On the other hand, dark photons are typically linked to new forces interacting with dark matter, potentially explaining anomalies like the muon's anomalous magnetic moment. Therefore, while sterile neutrinos can play a role in dark matter models, dark photons are more related to new forces and interactions within the dark sector, highlighting the distinction between these two hypothetical particles.
What is the latest cosmological constraints on the gravity theory?
5 answers
The latest cosmological constraints on gravity theories involve the investigation of torsional modifications of general relativity, specifically $f(T)$ gravity. By utilizing data from Pantheon supernovae, Baryon Acoustic Oscillations (BAO), Big Bang Nucleosynthesis (BBN), and Cosmic Microwave Background (CMB) observations, significant constraints have been placed on the effective parameters of $f(T)$ gravity models. Additionally, a novel test using large-scale structure data from the Baryon Oscillation Spectroscopic Survey (BOSS) has provided lower bounds on parameters characterizing the time evolution of the velocity field, indicating consistency with General Relativity predictions. These recent analyses represent substantial advancements in understanding the behavior of gravity at cosmological scales.
What are the physical and chemical properties of the milky sea phenomenon?
5 answers
The milky sea phenomenon is characterized by a widespread, uniform, and steady whitish glow on the ocean surface, resembling a daylit snowfield. This glow can cover massive areas exceeding 100,000 km2, persisting for days to weeks in specific oceanic regions with isolated water masses. Chemical analysis of milky waters in the North Sea revealed high oil content mainly composed of wax esters, similar to those found in copepods, suggesting a link to copepod mortality events. Additionally, the decomposition of green algae Ulva in shallow waters can lead to milky water conditions, characterized by low oxygen levels, a cream color, and the release of hydrogen sulfide, posing risks to marine life and causing unpleasant odors. These diverse physical and chemical properties contribute to the enigmatic nature of milky seas.
How does feedback affect galaxy formation and evolution?
5 answers
Feedback mechanisms, such as kinetic feedback from supernovae and AGN winds, significantly influence galaxy formation and evolution. Strong feedback reduces stellar mass in galaxies, aligning the stellar-mass-halo-mass relation with abundance matching results. It also impacts the morphology of low-mass galaxies, making them more elongated. Feedback processes regulate star formation, with AGN winds enhancing star formation in surrounding rings. The interplay between AGN wind power, star formation rate, and feedback phases shapes outflows and affects the efficiency of mass transport. Additionally, the relative contributions of black hole feedback and stellar feedback vary with galaxy mass, influencing the quenching or star-forming nature of galaxies. Overall, feedback mechanisms play a crucial role in shaping the properties and evolution of galaxies by impacting star formation, morphology, and mass transport.