A Service Mesh for Collaboration Between Geo-Distributed Services: The Replication Case

Mapping Intimacies ◽

10.1007/978-3-030-88583-0_17 ◽

2021 ◽

pp. 176-185

Author(s):

Marie Delavergne ◽

Ronan-Alexandre Cherrueau ◽

Adrien Lebre

Keyword(s):

Edge Computing ◽

Distributed Services ◽

Work In Progress

AbstractEdge computing is becoming more and more present, with sites geo-distributed around the globe. Applications on these infrastructures must be able to manage the latency and disconnections inherent to their distribution. One way to deal with these concerns could be to deploy one entire instance of the application per site and use a service mesh to manage the collaboration between the geo-distributed instances. More precisely, we propose to reify the location of application instances in REST requests and allow redirections between these requests thanks to a dedicated language and a service mesh allowing three types of collaborations. This paper focuses on the replication of a resource between multiple instances. Though it is still a work in progress, we demonstrated the relevance of our approach in the OpenStack ecosystem.

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Meridional Circulation, Turbulence, and Diffusion Processes in Stars

International Astronomical Union Colloquium ◽

10.1017/s0252921100080477 ◽

1976 ◽

Vol 32 ◽

pp. 109-116 ◽

Cited By ~ 1

Author(s):

S. Vauclair

Keyword(s):

Convection Zone ◽

Diffusion Processes ◽

Meridional Circulation ◽

Diffusion Time ◽

Work In Progress ◽

First Results ◽

Stellar Envelopes ◽

And Diffusion ◽

Turbulence And Diffusion ◽

Hr Diagram

This paper gives the first results of a work in progress, in collaboration with G. Michaud and G. Vauclair. It is a first attempt to compute the effects of meridional circulation and turbulence on diffusion processes in stellar envelopes. Computations have been made for a 2 Mʘstar, which lies in the Am - δ Scuti region of the HR diagram.Let us recall that in Am stars diffusion cannot occur between the two outer convection zones, contrary to what was assumed by Watson (1970, 1971) and Smith (1971), since they are linked by overshooting (Latour, 1972; Toomre et al., 1975). But diffusion may occur at the bottom of the second convection zone. According to Vauclair et al. (1974), the second convection zone, due to He II ionization, disappears after a time equal to the helium diffusion time, and then diffusion may happen at the bottom of the first convection zone, so that the arguments by Watson and Smith are preserved.

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