<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mmultiscripts><mml:mrow><mml:mi mathvariant="normal">He</mml:mi></mml:mrow><mml:mprescripts /><mml:mrow /><mml:mrow><mml:mn>3</mml:mn></mml:mrow><mml:mrow /><mml:mrow /></mml:mmultiscripts></mml:mrow></mml:math>(p,2p)d and<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mmultiscripts><mml:mrow><mml:mi mathvariant="normal">He</mml:mi></mml:mrow><mml:mprescripts /><mml:mrow /><mml:

Epstein, M. B.; Krause, Daniel; Margaziotis, D. J.; Bracco, A.; Gubler, H.P.; Hasell, D.; Lee, W. P.; Oers, W. T. H. van; Abegg, R.; Miller, C. A.; Stetz, A.W.

doi:10.1103/physrevc.32.967

Cited by 22 publications

(10 citation statements)

References 28 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The spectral functions S N (E, q) extracted by the plane-wave impulse approximation (PWIA) analysis from the 3 He(e, ep) [17], 3 He(p, 2p)d, and 3 He(p, pd)p reactions [18], were found to be in a reasonable agreement.…”

Section: Thesupporting

confidence: 51%

Analyzing powers Ayy , Axx , Axz and Ay in the dd → 3Hen reaction at 270 MeV

Janek¹,

Saito

Ladygin³

et al. 2007

Eur. Phys. J. A

View full text Add to dashboard Cite

Abstract. The data on the tensor Ayy, Axx, Axz and vector Ay analyzing powers in the dd → 3 Hen obtained at T d = 270 MeV in the angular range 0• -110• in the c.m. are presented. The observed negative sign of the tensor analyzing powers Ayy, Axx and Axz at small angles clearly demonstrate the sensitivity to the ratio of the D and S wave component of the 3 He wave function. However, the one-nucleon exchange calculations by using the standard 3 He wave functions have failed to reproduce the strong variation of the tensor analyzing powers as a function of the angle in the c.m.PACS. 24.70.+s Polarization phenomena in reactions -25.10.+s Nuclear reactions involving few-nucleon system -21.45.+v Few-body systems

show abstract

Section: Thesupporting

confidence: 51%

Analyzing powers Ayy , Axx , Axz and Ay in the dd → 3Hen reaction at 270 MeV

Janek¹,

Saito

Ladygin³

et al. 2007

Eur. Phys. J. A

View full text Add to dashboard Cite

show abstract

“…The dependence of t s on the gas density and relative streaming velocity |u − v| is determined by the grain size R d and the gas mean free path λ mfp . If R d 9λ mfp /4 the grains are in the Epstein regime (Epstein 1923;Baines et al 1965;Draine & Salpeter 1979), with…”

Section: Gas-dust Dragmentioning

confidence: 99%

Resonant drag instabilities in protoplanetary discs: the streaming instability and new, faster growing instabilities

Squire

Hopkins

2018

Monthly Notices of the Royal Astronomical Society

116

110

View full text Add to dashboard Cite

We identify and study a number of new, rapidly growing instabilities of dust grains in protoplanetary disks, which may be important for planetesimal formation. The study is based on the recognition that dust-gas mixtures are generically unstable to a Resonant Drag Instability (RDI), whenever the gas, absent dust, supports undamped linear modes. We show that the "streaming instability" is an RDI associated with epicyclic oscillations; this provides simple interpretations for its mechanisms and accurate analytic expressions for its growth rates and fastest-growing wavelengths. We extend this analysis to more general dust streaming motions and other waves, including buoyancy and magnetohydrodynamic oscillations, finding various new instabilities. Most importantly, we identify the disk "settling instability," which occurs as dust settles vertically into the midplane of a rotating disk. For small grains, this instability grows many orders of magnitude faster than the standard streaming instability, with a growth rate that is independent of grain size. Growth timescales for realistic dust-to-gas ratios are comparable to the disk orbital period, and the characteristic wavelengths are more than an order of magnitude larger than the streaming instability (allowing the instability to concentrate larger masses). This suggests that in the process of settling, dust will band into rings then filaments or clumps, potentially seeding dust traps, high-metallicity regions that in turn seed the streaming instability, or even overdensities that coagulate or directly collapse to planetesimals.

show abstract

“…Therefore the transition matrix element contains a purely nuclear structure element $(p3). This function P(p3) has been determined in He directly by pion absorption experiments [1] and with other probes [21,22,27,28]. [33] point out that a signature of an initial-state interaction as part of a two-step process would be a peak in the mass spectrum of the exchanged particle.…”

Section: Empty-target Subtractionmentioning

confidence: 99%

“…Figure 16 shows the Dalitz plot and its projections for a typical 2NA sensitive counter setup (XVII, in Table TABLE XI (26) assuming that the spectator nucleon is in a relative s-state to the absorbing nucleon pair. Our resulting five-fold differential cross section is then given by d CT dQdQ1 d O, d Qzdp3 (27) with p~h, being the phase-space factor, P(8) a function that depends on the neutron emission angle, and P(p3) the nucleon momentum probability density. Integration of the five-fold differential cross section over dQ& and d Qz over the surfaces of the two detectors and division XI).…”

Section: The H(m + Pp ) Reactionmentioning

confidence: 99%

Pion absorption in tritium at intermediate energies

et al. 1992

View full text Add to dashboard Cite

The angular distribution of nucleons from a kinematically complete measurement of pions absorbed in H on nucleon pairs with isospin T =0 and T = 1 at incident pion energies of 119, 206, and 300 MeV are presented. The T =0 data are quite similar to pion absorption data in deuterium. The integrated absorption cross sections scale within errors with the number of isoscaler neutron-proton pairs. The T =1 cross sections, which correspond to absorption on dineutrons, are an order of magnitude smaller. The angular distributions for isovector absorption show a significant asymmetry, indicating interference effects between amplitudes with or without b isobars in the intermediate states. The existence of a significant three-nucleon absorption component is established. The integrated absorption cross sections for processes involving two and three nucleons were determined. The neutron and proton momentum probability densities in H were determined from the spectator recoil resulting from quasifree twonucleon pion absorption.PACS number(s): 25.80.Ls, 25.10.+s

show abstract

He3(p,2p)d andHe

Cited by 22 publications

References 28 publications

Analyzing powers Ayy , Axx , Axz and Ay in the dd → 3Hen reaction at 270 MeV

Analyzing powers Ayy , Axx , Axz and Ay in the dd → 3Hen reaction at 270 MeV

Resonant drag instabilities in protoplanetary discs: the streaming instability and new, faster growing instabilities

Pion absorption in tritium at intermediate energies

Contact Info

Product

Resources

About