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If anyone knows plz let me know ASAP. ... I think u can use ASP.NET Membership, you can then place the UNprotected pdf files in a separate folder and deny the anonymous access to that folder... ... PdfDocumentSecurity security = new PdfDocumeentSecurity("1234"); //Load the PDF file with ... add password to pdf c# PDF Security Remover - CodeProject
4 Dec 2008 ... Remove security from PDF files. ... tested, but has worked on any PDF file that was marked Secure that I was able to open without a password . Following a visual brightness increase, Schulte-Ladbeck, Clayton & Meade (1993) undertook spectropolarimetry of the luminous blue variable (LBV) star, AG Car, and the LMC variable, R 127 For AG Car, the position angle of he intrinsic polarization is aligned with a major axis of the ring nebula and perpendicular to the jet In R 127, the polarization is perpendicular to two bright features of the local material These observations provide strong evidence that the asymmetries seen in the surroundings of these LBVs originate in the underlying stars AG Car became the subject of a more detailed paper by Schulte-Ladbeck, Clayton, Hillier, et al (1994) The H emission line pro le exhibits very extended wings that are differently polarized in amount and position angle relative to both the line core and the continuum, suggesting an origin by electron scattering in a dense wind The polarization exhibits large temporal variations indicating signi cant variations in the envelope opacity The general polarization varies along a preferred position angle of 145 , this direction interpreted as a symmetry axis of the stellar wind Its direction is co-aligned with the major axis of the AG Car ring nebula and perpendicular to the star s jet The temporal polarization variability of AG Car was con rmed by Leitherer, Allen, Altner, et al (1994), who also extended the polarimetry of this object into the ultraviolet Schulte-Ladbeck, Leitherer, Clayton, et al (1993) undertook colour lter measurements of R 127 in the Large Magellanic Cloud The polarization at H decreased with respect to the continuum They assumed that H line is recombination dominated, and thus intrinsically unpolarized, so allowing the interstellar polarization to be estimated The intrinsic polarization was determined to be of the order of 1% ! 15%, implying both the presence of copious free electrons and a considerable asphericity in their distribution Parthasarathy, Jain & Bhatt (2000) have made UBVRI measurements of HR Car, and noted large temporal changes in the level of p, and also in the form of p ( ) Spectropolarimetry of this object was also conducted by Clampin, Schulte-Ladbeck, Nota, et al (1995) Changes of polarization across the H emission line were noted Both these papers imply that the scattering material close to the star does not have a spherically symmetrical distribution, and that the behaviour is consistent with the bi-polar geometry imaged by others using a coronographic technique Spectropolarimetry has been undertaken of LBVs in our Galaxy and in the Magellanic Clouds by Davies, Oudmaijer & Vink (2005) They showed that many of their selected objects exhibit polarimetric signatures across the H emission line, indicating that the light from the stars is intrinsically polarized, and that asphericity already exists at the base of the wind Four of the target stars displayed polarization variability with three of them, AG Car, HR Car and P Cyg, providing temporal position angle changes which appeared random Such behaviour can be explained by the presence of strong wind-inhomogeneities, or clumps within the wind Only one star, R 127, exhibited p variations along an intrinsic line, with evidence of axial symmetry, as well as clumpiness However, if viewed at low inclination, and with limited temporal sampling, such a wind would produce a seemingly random polarization of the type observed in the other three stars. remove password from pdf using c#: C# PDF Password Library: add, remove, edit PDF file password in ... c# itextsharp pdfreader not opened with owner password C# - remove password protection from PDF document ...
C# – remove password protection from PDF document. Updated on October 1, 2015 Kisan Patel. Problem: How to remove password protection from PDF ... remove pdf password c# How to protect PDF with password using C# , VB.NET | WinForms ...
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The temporal variation of p ( ) of R CrB itself was observed by Coyne & Shawl (1973) during a photometric minimum Very signi cant developments in the spectral behaviour were recorded, these being interpreted as dramatic changes in the distribution of particles of different sizes associated with the discrete cloud model Further observations were presented by Coyne (1974), which supported the model Spectropolarimetric observations have been made of V 854 Cen by Kameswara Rao & Raveendran (1993) They noted that the p ( ) variation was much steeper during the light minimum During the brightness decline phase, the polarized ux was attenuated by the same factor as the ux directly from the star, this implying that the obscuring cloud affects both the radiation from the photosphere and the scattering centres, suggesting a restriction to the geometrical extent of the scattering region In an observational study of the global values of p in a collection of objects in the stages of evolution from red giant to planetary nebula, Johnson & Jones (1991) noted that polarization is a characteristic of the majority of these stars When arranged on an evolutionary sequence, a clear trend in p was found A maximum of polarization was observed within an evolutionary stage The value of p was found to increase with age from mildly dusty Mira variables, through to protoplanetary nebulae for which the highest polarization is found; the polarization then decreases as the star evolves into an old planetary nebula Spectropolarimetry of 31 post-asymptotic giant branch (post-AGB) stars were observed by Trammell, Dinerstein & Goodrich (1994), these objects believed to be in the rst phases of the transition from the AGB to the planetary nebula stage Their survey suggested that the objects might be placed into one of four types depending on the recorded behaviour of p ( ) and ( ) Type [1] objects display higher levels of polarization and large position angle rotations; Type [2] have polarizations too large to be attributed to interstellar material, but without large position angle changes; Type [3] objects show position angle rotations nd polarization changes across TiO absorption features; Type [4] are objects for which the observed polarization can be entirely attributed to interstellar effects Twenty four objects displayed evidence for aspherical geometry, with an implication that asymmetry begins very early in the transition from AGB to the planetary nebula phase Their schematic model involves bipolar lobes giving rise to polarization in the blue part of the spectrum as a result of scattering of photospheric light by the contained dust grains Orthogonal to these lobes is an obscuring torus, and the polarization in the red is the result of scattering of photospheric light or transmission polarization in this torus Likkel, Morris, Kastner, et al (1994) have obtained maps of IRAS 21282+5050 revealing that the polarization is not centro-symmetric close into the stellar source It was concluded that there is not a large component of scattered light in the nearinfrared The emission at 22 m may arise from transiently heated dust In a polarimetric study of IRC +10216, a carbon-rich infrared evolved star on the AGB of the HR diagram, Kastner & Weintraub (1994) found elliptical symmetry in a J-band map endorsing other photometric maps, all these providing evidence of axial symmetry of the envelope, with the equatorial plane of the star lying perpendicular to the major axis of the surrounding inner envelope of the nebula The axisymmetric. 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