he public's desire for mobile communications and computing, as evidenced by the popularity of cellular phones, pagers, and laptop computers, combined with the rapid growth in demand for Internet access, suggest a very promising future for wireless data services. The key to realizing this potential is the development and deployment of high-performance radio systems. While many proposals for thir...

We present results of a recent Chandra X-ray Observatory observation of the central compact object (CCO) in the supernova remnant Cassiopeia A. This observation was obtained in an instrumental configuration that combines a high spatial resolution with a minimum spectral distortion, and it allowed us to search for pulsations with periods longer than ≈ 0.68 s. We found no evidence of extended emi...

There are ∼ 1, 0.1 and 0.01 gravitationally lensed X-ray sources per square degree with soft X-ray fluxes exceeding 10 −15 , 10 −14 and 10 −13 ergs s −1 cm −2 respectively. These sources will be detected serendipitously with the Chandra X-ray Observatory at a rate of 1–3 lenses per year of high resolution imaging. The low detection rate is due to the small area over which the HRC and ACIS camer...

We present six Chandra X-ray spectra and light curves obtained for the nova V1494Aql (1999 #2) in outburst. The first three observations were taken with ACIS-I on days 134, 187, and 248 after outburst. The count rates were 1.00, 0.69 and 0.53 cps, respectively. We found no significant periodicity in the ACIS light curves. The X-ray spectra show continuum emission and lines originating from N an...

We report the first unambiguous detection of X-ray emission originating from Saturn with a Chandra observation, duration 65.5 ksec with ACIS-S3. Beyond the pure detection we analyze the spatial distribution of X-rays on the planetary surface, the light curve, and some spectral properties. The detection is based on 162 cts extracted from the ACIS-S3 chip within the optical disk of Saturn. We fou...

In this document we compare event detection e ciencies in the TE mode to the ones expected in the CC(1x3) mode in the ACIS-S detector array of the HETG spectrometer on board the Chandra X-ray Observatory. Data taken in TE mode have pulse heights determined from the charge in a 3x3 pixel event island. In CC(1x3) mode, events are read out on a row by row basis, and therefore the pulse height for ...

هدف: هدف از پژوهش حاضر مقایسۀ واکنش ­پذیری هیجانی و نظریه ذهن کودکان بر اساس سبک ­های ابرازگری مادرانشان بود. روش: روش توصیفی نوع علّی-مقایسه­ ای بود در دو گام به صورت آنلاین انجام رسید. ابتدا با استفاده نمونه ­گیری دسترس، تعداد 105 نفر مادرانی که نمرات آن­ها هر یک پرسشنامه کینگ امونز (1990)، دوسوگرایی (1990) کنترل راجر نشوور (1987) انحراف استاندارد بالاتر میانگین دست آمد (در گروه 35 نفر) دوم وا...