Hole scattering mechanism of strained Si/(111)Si1−x Ge x

Wang, Cheng; Zhang, Heming; Song, Jianjun; Hu, Huiyong

doi:10.1007/s11433-011-4459-x

Cited by 4 publications

(3 citation statements)

References 11 publications

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“…Generally, the multipactor effect is strongly related to the secondary electron yield (SEY) of the materials. [10][11][12] The two most commonly used methods to suppress SEY effects are micro-trapping structure surface [13][14][15][16][17] and surface coating with low SEY materials. [8] Ye et al reduced the maximum secondary electron emission coefficient (δ max ) by 60% by fabricating the triangular raised structures.…”

Section: Introductionmentioning

confidence: 99%

Effect of Cu doping on the secondary electron yield of carbon films on Ag-plated aluminum alloy

Hu¹,

Zhu²,

Zhao³

et al. 2022

Chinese Phys. B

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Reducing the secondary electron yield (SEY) of Ag-plated aluminum alloy is important for high-power microwave components. In this work, Cu doped carbon films are prepared and the secondary electron emission characteristics are studied systematically. The secondary electron coefficient δ max of carbon films increases with the Cu contents increasing at first, and then decreases to 1.53 at a high doping ratio of 0.645. From the viewpoint of surface structure, the higher the content of Cu is, the rougher the surface is, since more cluster particles appear on the surface due to the small solid solubility of Cu in the amorphous carbon network. However, from viewpoint of the electronic structure, the reduction of the sp2 hybrid bonds will increase the SEY effect as the content of Cu increases, due to the decreasing probability of collision with free electrons. Thus, the two mechanisms would compete and coexist to affect the SEY characteristics in Cu doped carbon films.

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Section: Introductionmentioning

confidence: 99%

Effect of Cu doping on the secondary electron yield of carbon films on Ag-plated aluminum alloy

Hu¹,

Zhu²,

Zhao³

et al. 2022

Chinese Phys. B

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“…On the other hand, along with the rapid growth of the number of SN Ia discovered, the studies on the systematic uncertainties of SN Ia have drawn more and more attention. It has been proved that [21], the classic SN Ia statistics method (hereafter we will call it 'magnitude statistic' (MS)) suffers from various systematic uncertainties, such as the calibration errors [17], the host-galaxy extinction [22][23][24], the gravitational lensing [25,26], different light-curve fitters [27] and the redshift evolution of SN color-luminosity parameter β [28][29][30][31][32][33][34]. Therefore, the control of the systematic uncertainties of SN Ia have become one of the biggest challenges in SN cosmology.…”

Section: Introductionmentioning

confidence: 99%

Exploring the latest Pantheon SN Ia dataset by using three kinds of statistics techniques

Wang¹,

Luo²

2021

Commun. Theor. Phys.

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In this work, we explore the cosmological consequences of the latest Type Ia supernova (SN Ia) dataset, Pantheon, by adopting the wCDM model. The Pantheon dataset currently contains the largest number of SN Ia samples, which contains 1048 supernovae on the redshift range 0 < z < 2.3. Here we take into account three kinds of SN Ia statistics techniques, including: (1) magnitude statistics (MS), which is the traditional SN Ia statistics technique; (2) flux statistics (FS), which is based on the flux-averaging (FA) method; and (3) improved flux statistics (IFS), which combines the advantages of MS and FS. It should be mentioned that the IFS technique needs to scan the (z cut, Δz) parameters plane, where z cut and Δz are redshift cut-off and redshift interval of FA, respectively. The results are as follows. (1) Using the SN dataset only, the best FA recipe for IFS is (z cut, Δz) = (0.1, 0.08); (2) comparing to the old SN dataset, JLA, adopting the Pantheon dataset can reduce the 2σ error bars of equation of state w by 38%, 47% and 53% for MS, FS and IFS, respectively; (3) FS gives closer results to other observations, such as Baryon acoustic oscillations and cosmic microwave background; (4) compared with FS and IFS, MS more favors a Universe that will end in a ‘big rip’.

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“…Therefore, we wish to investigate the impacts of dark energy on constraining the total neutrino mass. In this work, we consider some typical dark energy models, including the ΛCDM model, the wCDM model, the w 0 w a CDM model (also known as the Chevallier-Polarski-Linder model or the CPL model) [13,14], and the holographic dark energy (HDE) model [15][16][17][18][19][20][21][22]. In addition, we also consider the effects from the neutrino mass hierarchies (i.e.…”

mentioning

confidence: 99%

Impacts of dark energy on constraining neutrino mass after Planck 2018

Zhang¹,

Zhang²,

Zhang³

2020

Commun. Theor. Phys.

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Considering the mass splittings of three active neutrinos, we investigate how the properties of dark energy affect the cosmological constraints on the total neutrino mass ∑ m ν using the latest cosmological observations. In this paper, several typical dark energy models, including ΛCDM, wCDM, CPL, and HDE models, are discussed. In the analysis, we also consider the effects from the neutrino mass hierarchies, i.e. the degenerate hierarchy (DH), the normal hierarchy (NH), and the inverted hierarchy (IH). We employ the current cosmological observations to do the analysis, including the Planck 2018 temperature and polarization power spectra, the baryon acoustic oscillations (BAO), the type Ia supernovae (SNe), and the Hubble constant H 0 measurement. In the ΛCDM+ ∑ m ν model, we obtain the upper limits of the neutrino mass ∑ m ν < 0.123 eV (DH), ∑ m ν < 0.156 eV (NH), and ∑ m ν < 0.185 eV (IH) at the 95% C.L., using the Planck+BAO+SNe data combination. For the wCDM+ ∑ m ν model and the CPL+ ∑ m ν model, larger upper limits of ∑ m ν are obtained compared to those of the ΛCDM+ ∑ m ν model. The most stringent constraint on the neutrino mass, ∑ m ν < 0.080 eV (DH), is derived in the HDE+ ∑ m ν model. In addition, we find that the inclusion of the local measurement of the Hubble constant in the data combination leads to tighter constraints on the total neutrino mass in all these dark energy models.

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Hole scattering mechanism of strained Si/(111)Si1−x Ge x

Cited by 4 publications

References 11 publications

Effect of Cu doping on the secondary electron yield of carbon films on Ag-plated aluminum alloy

Effect of Cu doping on the secondary electron yield of carbon films on Ag-plated aluminum alloy

Exploring the latest Pantheon SN Ia dataset by using three kinds of statistics techniques

Impacts of dark energy on constraining neutrino mass after Planck 2018

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