Incompressible analytical models for spinning-down pulsars
نویسندگان
چکیده
منابع مشابه
Too much pasta for pulsars to spin down
The lack of X-ray pulsars with spin periods > 12 s raises the question about where the population of evolved high magnetic field neutron stars has gone. Unlike canonical radio-pulsars, X-ray pulsars are not subject to physical limits to the emission mechanism nor observational biases against the detection of sources with longer periods. Here we show that a highly resistive layer in the innermos...
متن کاملRing-down absorption spectroscopy for analytical microdevices
In recent years, microfluidic separation techniques have changed the face of analytical chemistry. For example, capillary electrophoresis (CE) has greatly enhanced the sequencing of the human genome [1] and microfluidic chips have permitted not only chemical separation of nanolitersized, complex mixtures [2] but also highthroughput chemical reactions [3]. The main advantages of microfluidic dev...
متن کاملa new approach to credibility premium for zero-inflated poisson models for panel data
هدف اصلی از این تحقیق به دست آوردن و مقایسه حق بیمه باورمندی در مدل های شمارشی گزارش نشده برای داده های طولی می باشد. در این تحقیق حق بیمه های پبش گویی بر اساس توابع ضرر مربع خطا و نمایی محاسبه شده و با هم مقایسه می شود. تمایل به گرفتن پاداش و جایزه یکی از دلایل مهم برای گزارش ندادن تصادفات می باشد و افراد برای استفاده از تخفیف اغلب از گزارش تصادفات با هزینه پائین خودداری می کنند، در این تحقیق ...
15 صفحه اولPreconditioning Strategies for Models of Incompressible Flow
We describe some new preconditioning strategies for handling the algebraic systems of equations that arise from discretization of the incompressible Navier-Stokes equations. We demonstrate how these methods adapt in a straightforward manner to decisions on implicit or explicit time discretization, explore their use on a collection of benchmark problems, and show how they relate to classical tec...
متن کاملVariational models for the incompressible Euler equations
where ν is the unit exterior normal to ∂D. If v = (v, . . . , v) : [0, T ] ×D → R, then (adopting the summation convention) div v = ∂jv is the spatial divergence of v, ∇v is the spatial gradient, and ( v · ∇ ) v is the vector in R whose i-th component is given by v∂jv . Hence, (1.1) is a system of (d + 1) equations for the (d + 1) unknowns (v, . . . , v, p), where p : [0, T ] ×D → R physically ...
متن کاملذخیره در منابع من
با ذخیره ی این منبع در منابع من، دسترسی به آن را برای استفاده های بعدی آسان تر کنید
ژورنال
عنوان ژورنال: Publications of the Astronomical Society of Australia
سال: 2019
ISSN: 1323-3580,1448-6083
DOI: 10.1017/pasa.2019.28