Dünya'ya En Yakın Nötron Yıldızı <RX J1856>

Abstract

Comparing on RX J185635-3754 Neutron Star on optical and X-ray for 1°view with other rays taken from satallites and reseaƩrching on where it borns alculating excess flux of RX J1856 optical flux (49eV) to x-ray blacbody flux (57eV) discussing. DATAS FROM SATALLITES:*RASS-Cnt Broad, PSPC 2.0 Deg-Inten, Old PSPC (deg), COBE DIRBE, IRAS 12 micron, IRAS 100 micron, 1420 Mhz (Bonn) and GB6 (4850 MHz) are taken at 1°view, By using engtral we can calculate the areas under graphics; Excess flux=Ʃflux (upper)- Ʃflux (lower) The difference flux=(observed flux) – (x-rays for black body line continues) The upper line (observed) in between λ₁- λ₂ wavelength bands shows total flux from the target The upper line ( X-rays for black body line continues) in between λ₁- λ₂ wavelength bands shows tolal flux from a black body, Excess flux of optical spectral energy distribution flux to x-ray for blackbody energy distribution flux (57 eV) [Between F303 HSTU and F606 HSTV] Corpared to binary X-ray pulsars, AXPs have lower luminosities and exhisits narrow distiribution of periods. Unlike young radio pulsars, AXPs have rather long periods and appear to be radio quiet. To understanding there differences is to try and identfy the energy source that powers the x-ray emmision. It is quite clear that this energy can’t be provided by rotation. Their rotating speed is too more, after the explosion the conductive liquid matter inside the star causes 1 x 10¹² Gauss Magnetic Field that makes the star like a dynamoMagnetars: X-ray luminosities could be powered by magnetic field. Residual thermal energy ( if it is correct the envolope of the star must consist light elements such as hyrdogen and helium). The emission is powered by magnetic field deray then a value of B≥10¹⁶ G is requried unlies nonstandart deray processes are invoked As AXPs models it’s alone, SGR models it’s magnetar, SGR and AXP common properties it’s alone and in AXP and SGR it is 10⁶ year old. As AXP DNT SGR RQNSS it’s propeller spindown with high spindown rates larger than 10-12 rad/s² can indeed be expected for neutron stars with conventinal 10¹² Gauss fields under the typical spindown torques for certain phases of accreting sources. Propeller torques depend on the magnetic moment of the neutron star and on the rate of mass in flow.