How to Reduce Attrition in Company X?

Attrition is one of the biggest issues requiring improvement at Company X like in its field of business in general. Many people that apply to contact center field are searching for a short-term employment only. In order to reduce attrition, it is important to acknowledge the real reasons why an employee decides to resign. This study concentrates on the factors that most effect on the decision to resign and tries to go deeper. The objective of this study was to find out the real reasons behind an employee’s decision to resign and collect improvement ideas or methods to decrease the amount of yearly resignations at Company X. In addition to theoretical frame of reference, the study is based on qualitative analysis. During 3 months the exiting employees answered an anonymous questionnaire and 22 were interviewed in person. Written data was collected from 18 respondents. The questions were related to one’s experience on atmosphere, image of work content before and after employment, supervisors, training, scheduling and so on. Majority of respondents stated that Company X was a good employer. Issues that affected on the decision to leave were lack of time (students) and issues with supervisors. The most common reason mentioned, was the monotonous work content. Work content was not mentioned as the main reason, however, but a reason effecting the decision. Main reasons were mostly studies, uncompetitive salary or lack of feel of success. In order to decrease the level attrition at a company like Company X, the employer must affect on employees’ motivation and gain commitment though motivated employees. Company X conducts certain researches for their personnel regularly and are therefore well aware of points of improvements. According to the results gathered from this research, there is work to do to improve supervisors’ leadership skills. Also recognizing the signs before one decides to resign is important. By keeping up and improving the great working atmosphere and creating varying working possibilities, Company X can try to decrease attrition to the target level

ExploreNEOs: Average albedo by taxonomic complex in the near-Earth asteroid population

Understanding the albedo distribution of the near-Earth object (NEO) population allows for a better understanding of the relationship between absolute magnitude and size, which impacts calculations of size-frequency distribution and impact hazards. Examining NEO albedos also sheds light on the differences between the NEO and Main-Belt populations. We combine albedo results from the ExploreNEOs Warm Spitzer Exploration Science program with taxonomic classifications from the literature, publicly available datasets, and new observations from our concurrent spectral survey to derive the average albedos for C-, D-, Q-, S-, V- and X-complex NEOs

ExploreNEOs. V. Average Albedo by Taxonomic Complex in the Near-Earth Asteroid Population

Examining the albedo distribution of the near-Earth object (NEO) population allows for a better understanding of the relationship between absolute (H) magnitude and size, which impacts calculations of the size frequency distribution and impact hazards. Examining NEO albedos also sheds light on the differences between the NEO and Main Belt populations. We combine albedo results from the ExploreNEOs Warm Spitzer Exploration Science program with taxonomic classifications from the literature, publicly available data sets, and new observations from our concurrent spectral survey to derive the average albedos for C-, D-, Q-, S-, V-, and X-complex NEOs. Using a sample size of 118 NEOs, we calculate average albedos of 0.29+0.05 –0.04, 0.26+0.04 –0.03, and 0.42+0.13 –0.11 for the Q-, S-, and V-complexes, respectively. The averages for the C- and D-complexes are 0.13+0.06 –0.05 and 0.02+0.02 –0.01, but these averages are based on a small number of objects (five and two, respectively) and will improve with additional observations. We use albedos to assign X-complex asteroids to one of the E-, M-, or P-types. Our results demonstrate that the average albedos for the C-, S-, V-, and X-complexes are higher for NEOs than the corresponding averages observed in the Main Belt

ExploreNEOs: The Warm Spitzer near Earth object survey

We are carrying out the ExploreNEOs project in which we observe more than 600 near Earth Objects (NEOs) at 3.6 and 4.5 microns with Warm Spitzer. For each NEO we derive diameter and albedo. We present our results to date, which include studies of individual objects, results for our entire observed sample, and, by extrapolation, results for the entire NEO population. We also present several avenues of future work

Radar Observations and Physical Modeling of Asteroid 6489 Golevka

44> Author AC voice fax JPL E-mail mailstop ----------------------------------------------------------------------------- Hudson 509 335-0922 335-3818 [email protected] Ostro 818 354-3173 354-9476 300-233 [email protected] Jurgens 818 354-4974 354-6825 238-420 [email protected] Rosema 818 393-2629 354-9476 300-233 [email protected] Giorgini 818 393-3107 393-1159 301-150 [email protected] Winkler 760 255-8259 255-8515 DSCC-61 [email protected] Rose 760 255-8259 255-8515 DSCC-61 [email protected] Choate 760 255-8259 255-8515 DSCC-74 [email protected] Cormier 760 255-8358 255-8554 DSCC-74 [email protected] Franck 818 354-6842 354-6825 238-420 [email protected] Frye 818 354-6874 354-6825 238-420 [email protected] Howard 818 354-8753 354-8153 125-177 [email protected] Kelley 760 255-8358 255-8554 DSCC-74 [email protected] Littlefa

Photometric Survey of Binary Near-Earth Asteroids

Photometric data on 17 binary near-Earth asteroids (15 of them are certain detections, two are probables) were analysed and characteristic properties of the near-Earth asteroid (NEA) binary population were inferred. We have found that binary systems with a secondary-to-primary mean diameter ratio Ds/Dp > 0.18 concentrate among NEAs smaller than 2 km in diameter; the abundance of such binaries decreases significantly among larger NEAs. Secondaries show an upper size limit of Ds = 0.5–1 km. Systems with Ds/Dp < 0.5 are abundant but larger satellites are significantly less common. Primaries have spheroidal shapes and they rotate rapidly, with periods concentrating between 2.2 to 2.8 h and with a tail of the distribution up to ~4 h. The fast rotators are close to the critical spin for rubble piles with bulk densities about 2 g/cm3. Orbital periods show an apparent cut-off at Porb ~11 h; closer systems with shorter orbital periods have not been discovered, which is consistent with the Roche limit for strengthless bodies. Secondaries are more elongated on average than primaries. Most, but not all, of their rotations appear to be synchronized with the orbital motion; non-synchronous secondary rotations may occur especially among wider systems with Porb > 20 h. The specific total angular momentum of most of the binary systems is similar to within ±20% and close to the angular momentum of a sphere with the same total mass and density, rotating at the disruption limit; this suggests that the binaries were created by mechanism(s) related to rotation near the critical limit and that they neither gained nor lost significant amounts of angular momentum during or since formation. A comparison with six small asynchronous binaries detected in the main belt of asteroids suggests that the population extends beyond the region of terrestrial planets, but with characteristics shifted to larger sizes and longer periods. The estimated mean proportion of binaries with Ds/Dp > 0.18 among NEAs larger than 0.3 km is 15±4%. Among fastest rotating NEAs larger than 0.3 km with periods between 2.2-2.8 h, the mean proportion of such binaries is (66+10−12)%

Apophis Planetary Defense Campaign

We describe results of a planetary defense exercise conducted during the close approach to Earth by the near-Earth asteroid (99942) Apophis during 2020 December–2021 March. The planetary defense community has been conducting observational campaigns since 2017 to test the operational readiness of the global planetary defense capabilities. These community-led global exercises were carried out with the support of NASA’s Planetary Defense Coordination Office and the International Asteroid Warning Network. The Apophis campaign is the third in our series of planetary defense exercises. The goal of this campaign was to recover, track, and characterize Apophis as a potential impactor to exercise the planetary defense system including observations, hypothetical risk assessment and risk prediction, and hazard communication. Based on the campaign results, we present lessons learned about our ability to observe and model a potential impactor. Data products derived from astrometric observations were available for inclusion in our risk assessment model almost immediately, allowing real-time updates to the impact probability calculation and possible impact locations. An early NEOWISE diameter measurement provided a significant improvement in the uncertainty on the range of hypothetical impact outcomes. The availability of different characterization methods such as photometry, spectroscopy, and radar provided robustness to our ability to assess the potential impact risk. © 2022. The Author(s). Published by the American Astronomical Society.Open access journalThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at [email protected]