… In the following we will look at values of X(S,S * ) over various possible choices of string
pairs S and S * , and demonstrate that for inverse pairs they are distributed differently than for …

… At node n, for every element α in the node’s tail, a new node n is generated such that n .… a
threshold we set 10% - if the sparse bit vector contains less than 10% of ’1’s it will be projected. …

We present AIM2-F, an improved implementation of AIM-F [4] algorithm for mining frequent
itemsets. Past studies have proposed various algorithms and techniques for improving the …

… where M s and R s are the host star's (ie, the primary star's) mass and radius, respectively,
M 2 and R 2 are the secondary mass and radius, respectively, P orb , i and a are the orbital …

We report the discovery of a warm sub-Saturn, TOI-257b (HD 19916b), based on data from
NASA’s Transiting Exoplanet Survey Satellite (TESS). The transit signal was detected by …

We present the first measurement of the planet frequency beyond the “snow line,” for the
planet-to-star mass-ratio interval− 4. 5< log q<− 2, corresponding to the range of ice giants to …

… if the given pattern contains an increasing sequence of length s−γ. This task can be … s−γ
this is the longest increasing subsequence, otherwise no increasing subsequence of length s …

… We also present a new K s -band occultation observation of WASP-12b obtained with the
Palomar/Wide-field Infrared Camera instrument. The latest TESS photometry spans three …

… s and 4.5 μm bands in 2016 and 2017. The observed transit depths are different at these
wavelengths. However, after correcting for excess dust emission at K s … (with radii s ≲ 1.5 μm) in …

… of 9 s but decreased the exposure time incrementally to 8 s, 7 s, and finally 6 s throughout
the … beaming-based planet mass estimate compared to our results in Shporer et al. (2011). …