Sequencing the Stars
نویسنده
چکیده
It is easy to forget that less than 100 years ago, no one knew the process by which stars produce light. Today, we understand quite well that stars, which are composed mostly of hydrogen, produce energy by nuclear fusion. The enormous pressure created by the mass of a star causes pairs of hydrogen nuclei in its core to fuse into a helium nucleus thereby converting a small amount of mass into energy. Hence, we have starlight.
منابع مشابه
Pulsating red giant and supergiant stars in the Local Group dwarf galaxy Andromeda I
We have conducted an optical long-term monitoring survey of the majority of dwarf galaxies in the Local Group, with the Isaac Newton Telescope (INT), to identify the long period variable (LPV) stars. LPV stars vary on timescales of months to years, and reach the largest amplitudes of their brightness variations at optical wavelengths, due to the changing temperature. They trace stellar populati...
متن کاملLINEAR PULSATION CHARACTERISTICS OF MIRA VARIABLE STARS
The linear adiabatic pulsation-periods of Mira variable stars have been derived. Approximately 2701[1]models were calculated for M = 0.7 MΘ to 2 MΘ stars with radii from 180 RΘ to 340 RΘ and luminosities from 2800 LΘ to 10,000 LΘ. The chemical composition of all models is (X,Z) = (0.7,0.02). From the result of this study, linear relations on Luminosity-Period-Mass relationship and luminosity-pe...
متن کاملUnweighted p-center problem on extended stars
An extended star is a tree which has only one vertex with degree larger than two. The -center problem in a graph asks to find a subset of the vertices of of cardinality such that the maximum weighted distances from to all vertices is minimized. In this paper we consider the -center problem on the unweighted extended stars, and present some properties to find solution.
متن کاملارائه الگوریتم شناسایی ستاره بر مبنای رأی‌گیری هندسی به منظور استفاده در ردیاب‌های ستاره‌ای
Star identification is one of the most important stages in attitude determination with star trackers. This can be performed using matching algorithms between observed stars and a master star catalogue. The main challenge in this approach is to provide a fast and reliable identification algorithm that is sufficiently robust in different pointing views of the star tracker optical system in the sp...
متن کاملDifferent Magnetic Field Distributions in Deformed Neutron Stars
In this work, we review the formalism which would allow us to model magnetically deformed neutron stars. We study the effect of different magnetic field configurations on the equation of state (EoS) and the structure of such stars. For this aim, the EoS of magnetars is acquired by using the lowest order constraint variational (LOCV) method and employing the AV18 potential....
متن کاملSpin and Isospin Asymmetry, Equation of State and Neutron Stars
In the present work, we have obtained the equation of state for neutron star matter considering the in uence of the ferromagnetic and antiferromagnetic spin state. We have also investigated the structure of neutron stars. According to our results, the spin asymmetry stiens the equation of state and leads to high mass for the neutron star.
متن کاملذخیره در منابع من
با ذخیره ی این منبع در منابع من، دسترسی به آن را برای استفاده های بعدی آسان تر کنید
عنوان ژورنال:
دوره شماره
صفحات -
تاریخ انتشار 2013