Etnoconhecimento E Cultivo De Plantas Medicinais

Aprile, Fabio; Siqueira, Gilmar Wanzeller

doi:10.24824/978858042301.3

Cited by 33 publications

(51 citation statements)

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“…For comparison, the current limits and regions on σ p reported by various direct detection experiments are also shown in Fig. 3, including the regions from DAMA-Libra (Bernabei et al 2008) and CDMS-Si (Agnese & Ahmed et al 2013) experiments and the limits from Super-CDMS (Agnese et al 2014), XENON100 (Aprile et al 2012) and LUX (Akerib et al 2014) groups. Also included are the expected sensitivity of future experiment XENON1T (Aprile et al 2015) and the "neutrino discovery limit" (Billard et al 2014) which sets limit on the sensitivity of the direct detection method.…”

Section: Shown Inmentioning

confidence: 99%

“…For the SQS case, DM is assumed to only interact with the first family of quarks. The corresponding results from direct detection experiments, i.e., DAMA-Libra (Bernabei et al 2008), CDMS-II(Si) (Agnese & Ahmed et al 2013), XENON100 (Aprile et al 2012), LUX (Akerib et al 2014), SuperCDMS(Ge) (Agnese et al 2014) as well as the future XENON1T (Aprile et al 2015) and the "neutrino discovery limit" (Billard et al 2014) are also included for comparison.…”

Section: Shown Inmentioning

confidence: 99%

“…Among these works, the host compact stars are generally assumed to be neutron stars (NSs), and thus numerous constraints on DM-nucleon interactions have been obtained. In particular, for bosonic DM which is favored by many theories beyond the standard model, if its self-interactions can be ignored, the formation of Bose-Einstein condensate (BEC) state could further facilitate the occurrence of DM collapsing into BH, and the resulting limits on the DMnucleon interactions become far beyond the terrestrial experiments (Bernabei et al 2008;Aprile et al 2012;Akerib et al 2014;Agnese & Ahmed et al 2013;Agnese et al 2014;Aprile et al 2015;Billard et al 2014), leading to a conclusion that the bosonic DM cannot be detected directly if the old compact stars are NSs.…”

Section: Introductionmentioning

confidence: 99%

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Strange Quark Stars as a Probe of Dark Matter

Zheng

Chen

2016

ApJ

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We demonstrate that the observation of old strange quark stars (SQSs) can set important limits on the scattering cross sections σ q between the light quarks and the non-interacting scalar dark matter (DM). By analyzing a set of 1403 of solitary pulsarlike compact stars in the Milky Way, we find the old solitary pulsar PSR J1801-0857D can set the most stringent upper limits on σ q or the DM-proton scattering cross sections σ p . By converting σ q into σ p based on effective operator analyses, we show the resulting σ p limit by assuming PSR J1801-0857D to be a SQS could be comparable with that of the current direct detection experiments but much weaker (by several orders of magnitude) than that obtained by assuming PSR J1801-0857D to be a neutron star (NS), which requires an extremely small σ p far beyond the limits of direct detection experiments. Our findings imply that the old pulsars are favored to be SQSs rather than NSs if the scalar DM were observed by future terrestrial experiments.

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Section: Shown Inmentioning

confidence: 99%

Section: Shown Inmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Strange Quark Stars as a Probe of Dark Matter

Zheng

Chen

2016

ApJ

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“…Some with the cryogenic detector embody CDMS 13 , CRESST 14 , EDEDWEISS 15 , and EURECA 16 and so on. Some others with the cryogenic detector contain ZEPLIN 17 , XENON 18 , DEAP 19 , ArDM 20 , WARP 21 , DarkSide 22 , LUX 23 , and PandaX 24 and so forth. Other detection experiments include SIMPLE 25 and PICASSO 26 and so on.…”

Section: Dark Matter Detectionmentioning

confidence: 99%

Some properties of dark matter field in the complex octonion space

Weng

2015

Int. J. Mod. Phys. A

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The paper aims to consider the electromagnetic adjoint-field in the complex octonion space as the dark matter field, describing some properties of dark matter, especially the origin, particle category, existence region, and force and so forth. Since J. C. Maxwell applied the algebra of quaternions to depict the electromagnetic theory, some scholars adopt the complex quaternion and octonion to study the physics property of electromagnetic and gravitational fields. In the paper, by means of the octonion operator, it is found that the gravitational field accompanies with one adjoint-field, which property is partly similar to that of electromagnetic field. And the electromagnetic field accompanies with another adjoint-field, which feature is partly similar to that of gravitational field. As a result the electromagnetic adjoint-field is able to be chosen as one candidate of the dark matter field. According to the electromagnetic adjoint-field, it is able to predict a few properties of dark matter, for instance, the particle category, interaction intensity, interaction distance, and existence region and so forth. The study reveals that the dark matter particle and gravitational resource both will be influenced by the gravitational strength and force. The dark matter field is capable of making a contribution to physics quantities of gravitational field, including the angular momentum, torque, energy, and force and so on. Further there may be comparatively more chances to discover the dark matter in some regions with the ultrastrong field strength, surrounding the neutral star, white dwarf, galactic nucleus, black hole, and astrophysical jet and so on.Comment: A few minor changes in the second version, due to the typewriting erro

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“…The first two experiments use liquid xenon as their target material, inspired by the planned XENON1T and under-construction LUX experiments [29,72]. The third toy experiment is based on the several ton-scale liquid-argon experiments planned and under construction (e.g., the various experiments in the DEAP/CLEAN program [32], ArDM [31]).…”

Section: Toy Experimentsmentioning

confidence: 99%

WIMP astronomy and particle physics with liquid-noble and cryogenic direct-detection experiments

Peter

2011

Phys. Rev. D

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Once weakly-interacting massive particles (WIMPs) are unambiguously detected in directdetection experiments, the challenge will be to determine what one may infer from the data. Here, I examine the prospects for reconstructing the local speed distribution of WIMPs in addition to WIMP particle-physics properties (mass, cross sections) from next-generation cryogenic and liquidnoble direct-detection experiments. I find that the common method of fixing the form of the velocity distribution when estimating constraints on WIMP mass and cross sections means losing out on the information on the speed distribution contained in the data and may lead to biases in the inferred values of the particle-physics parameters. I show that using a more general, empirical form of the speed distribution can lead to good constraints on the speed distribution. Moreover, one can use Bayesian model selection criteria to determine if a theoretically-inspired functional form for the speed distribution (such as a Maxwell-Boltzmann distribution) fits better than an empirical model. The shape of the degeneracy between WIMP mass and cross sections and their offset from the true values of those parameters depends on the hypothesis for the speed distribution, which has significant implications for consistency checks between direct-detection and collider data. In addition, I find that the uncertainties on theoretical parameters depends sensitively on the upper end of the energy range used for WIMP searches. Better constraints on the WIMP particle-physics parameters and speed distribution are obtained if the WIMP search is extended to higher energy (∼ 1 MeV).

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Etnoconhecimento E Cultivo De Plantas Medicinais

Cited by 33 publications

References 0 publications

Strange Quark Stars as a Probe of Dark Matter

Strange Quark Stars as a Probe of Dark Matter

Some properties of dark matter field in the complex octonion space

WIMP astronomy and particle physics with liquid-noble and cryogenic direct-detection experiments

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