We report the discovery of HATS-71b, a transiting gas giant planet on a day orbit around a mag M3 dwarf star. HATS-71 is the coolest M dwarf star known to host a hot Jupiter. The loss of light during ...transits is 4.7%, more than in any other confirmed transiting planet system. The planet was identified as a candidate by the ground-based HATSouth transit survey. It was confirmed using ground-based photometry, spectroscopy, and imaging, as well as space-based photometry from the NASA Transiting Exoplanet Survey Satellite mission (TIC 234523599). Combining all of these data, and utilizing Gaia DR2, we find that the planet has a radius of and mass of (95% confidence upper limit of ), while the star has a mass of and a radius of .
We report the discovery of HAT-P-30b, a transiting exoplanet orbiting the V = 10.419 dwarf star GSC 0208-00722. The planet has a period P = 2.810595 ? 0.000005 days, transit epoch Tc = 2455456.46561 ...? 0.00037 (BJD), and transit duration 0.0887 ? 0.0015 days. The host star has a mass of 1.24 ? 0.04 M , radius of 1.21 ? 0.05 R , effective temperature of 6304 ? 88 K, and metallicity Fe/H = +0.13 ? 0.08. The planetary companion has a mass of 0.711 ? 0.028 M J and radius of 1.340 ? 0.065 R J yielding a mean density of 0.37 ? 0.05 g cm--3. We also present radial velocity measurements that were obtained throughout a transit that exhibit the Rossiter-McLaughlin effect. By modeling this effect, we measure an angle of Delta *l = 735 ? 90 between the sky projections of the planet's orbit normal and the star's spin axis. HAT-P-30b represents another example of a close-in planet on a highly tilted orbit, and conforms to the previously noted pattern that tilted orbits are more common around stars with T eff 6250 K.
We report the discovery of HAT-P-26b, a transiting extrasolar planet orbiting the moderately bright V = 11.744 K1 dwarf star GSC 0320--01027, with a period P = 4.234516 ? 0.000015 days, transit epoch ...Tc = 2455304.65122 ? 0.00035 (BJD; Barycentric Julian dates throughout the paper are calculated from Coordinated Universal Time (UTC)), and transit duration 0.1023 ? 0.0010 days. The host star has a mass of 0.82 ? 0.03 M , radius of 0.79+0.10 --0.04 R , effective temperature 5079 ? 88 K, and metallicity Fe/H = -0.04 ? 0.08. The planetary companion has a mass of 0.059 ? 0.007 M J, and radius of 0.565+0.072 --0.032 R J yielding a mean density of 0.40 ? 0.10 g cm-3. HAT-P-26b is the fourth Neptune-mass transiting planet discovered to date. It has a mass that is comparable to those of Neptune and Uranus, and slightly smaller than those of the other transiting Super-Neptunes, but a radius that is ~65% larger than those of Neptune and Uranus, and also larger than those of the other transiting Super-Neptunes. HAT-P-26b is consistent with theoretical models of an irradiated Neptune-mass planet with a 10 M {circled plus} heavy element core that comprises 50% of its mass with the remainder contained in a significant hydrogen-helium envelope, though the exact composition is uncertain as there are significant differences between various theoretical models at the Neptune-mass regime. The equatorial declination of the star makes it easily accessible to both Northern and Southern ground-based facilities for follow-up observations.
We report on the discovery of a planetary system with a close-in transiting hot Jupiter on a near circular orbit and a massive outer planet on a highly eccentric orbit. The inner planet, HAT-P-13b, ...transits the bright V = 10.622 G4 dwarf star GSC 3416 - 00543 every P = 2.916260 +/- 0.000010 days, with transit epoch Tc = 2454779.92979 +/- 0.00038 (BJD) and duration 0.1345 +/- 0.0017 days. The outer planet HAT-P-13c orbits the star every P 2 = 428.5 +/- 3.0 days with a nominal transit center (assuming zero impact parameter) of T 2c = 2454870.4 +/- 1.8 (BJD) or time of periastron passage T 2,peri = 2454890.05 +/- 0.48 (BJD). Transits of the outer planet have not been observed, and may not be present. The host star has a mass of 1.22+0.05 -0.10 M, radius of 1.56 +/- 0.08 R, effective temperature of 5653 +/- 90 K, and is rather metal-rich with Fe/H = +0.41 +/- 0.08. The inner planetary companion has a mass of 0.853+0.029 -0.046 M J, and radius of 1.281 +/- 0.079 R J, yielding a mean density of 0.498+0.103 -0.069 g cm-3. The outer companion has m 2sin i 2 = 15.2 +/- 1.0 M J, and orbits on a highly eccentric orbit of e 2 = 0.691 +/- 0.018. While we have not detected significant transit timing variations of HAT-P-13b, due to gravitational and light-travel time effects, future observations will constrain the orbital inclination of HAT-P-13c, along with its mutual inclination to HAT-P-13b. The HAT-P-13 (b, c) double-planet system may prove extremely valuable for theoretical studies of the formation and dynamics of planetary systems.
Abstract
Empty fruit bunches (EFB) contain macro and micronutrients, so they can be used as compost. EFB takes a long time to be composted because it has high cellulose. Used cellulolytic bacteria ...decomposers are a solution to boost EFB composting. The goal of this research is to get cellulolytic bacteria with a high potential for accelerating composting and producing high-quality compost. The study used a completely randomized design with several types of cellulolytic bacteria and was repeated three times. Data is presented in qualitative and quantitative formats. The qualitative data were analyzed descriptively, the quantitative data were analyzed using analysis of variance, and the Honestly Significant Difference (HSD) test was run at a 5% significance level. Temperature, volume shrinkage, color, smell, C-organic, N-total, C/N ratio, and pH parameters of the compost were analyzed. The results showed that the application of cellulolytic bacterial isolates could improve the quality of OPEFB compost (in accordance with SNI Compost Quality Standards: 19-7030-2004) and speed up composting time. Consortium I was the best treatment with reduced compost volume up to 74.53%, decreased C-organic content up to 23.32%, increased total N content up to 1.88% and decreased C/N ratio up to 12.44.
We report the discovery of HAT-P-27b, an exoplanet transiting the moderately bright G8 dwarf star GSC 0333-00351 (V = 12.214). The orbital period is 3.039586 ? 0.000012 days, the reference epoch of ...transit is 2455186.01879 ? 0.00054 (BJD), and the transit duration is 0.0705 ? 0.0019 days. The host star with its effective temperature 5300 ? 90 K is somewhat cooler than the Sun and is more metal-rich with a metallicity of +0.29 ? 0.10. Its mass is 0.94 ? 0.04 M and radius is 0.90+0.05 -- 0.04 R . For the planetary companion we determine a mass of 0.660 ? 0.033 M J and radius of 1.038+0.077 -- 0.058 R J. For the 30 known transiting exoplanets between 0.3 M J and 0.8 M J, a negative correlation between host star metallicity and planetary radius and an additional dependence of planetary radius on equilibrium temperature are confirmed at a high level of statistical significance.
As described in sect; 2.3, each HSsub 4 unit is controlled by a single control computer running Linux with a special kernel that is capable of real-time operations. In addition, a node-computer is ...responsible for weather sensing and synchronizing the time to the GPS time. A large suite of software is running on the control and node computers, responsible for the instrument control. We broadly classify the control software components to "low-level", meaning direct control of instruments, and "high-level", referring to more general observatory control, usually connected to the "low-level" software. The control of the telescope mount is performed through a Xenomai-based (real-time) character device driver, called the scope module. This module depends on the basic built-in printer port control modules of Linux. When the scope kernel module is loaded, a number of initial parameters are supplied, such as the choice of the hemisphere (to determine the direction of tracking), the resolution of the axes, settings for ramping up the motors to maximal slewing speed, and the level of verbosity.
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