Early evaluation of cocoa (Theobroma cacao L.) clones as intercrop in coconut gardens under red river region of Assam State, India

A field experiment was conducted at Horticultural Research Station (AICRP on Palms), Kahikuchi of Assam Agricultural University for three consecutive years (2018-20) to study the initial performance of cocoa clones as intercrop in adult coconut (Cocos nucifera L) garden spaced at 7.5 m × 7.5 m taking sixteen cocoa clones. Data on tree height, stem girth, number of pods, pod weight, number of beans pod-1, dry bean weight tree-1 year-1 and single dry bean weight revealed significant variations among the 16 cocoa clones. Dried beans are the prime economic produce of cocoa, and single dry bean weight ranged from 0.95 to 1.4 g. With respect to dry bean yield tree-1, VTLC-20 recorded a significantly higher dry bean yield of 2.2 kg tree-1 followed by VTLC-18 (1.5 kg tree-1) compared to other cocoa clones, and eight clones yielded more than 1.0 kg dry bean tree-1. Results showed that the number of leaves on the crown, number of inflorescences per palm and nut yield of coconut was not negatively affected; rather, there was an increase in the yield of coconut over a period

Observation of Gravitational Waves from Two Neutron Star-Black Hole Coalescences

We report the observation of gravitational waves from two compact binary coalescences in LIGO's and Virgo's third observing run with properties consistent with neutron star–black hole (NSBH) binaries. The two events are named GW200105_162426 and GW200115_042309, abbreviated as GW200105 and GW200115; the first was observed by LIGO Livingston and Virgo and the second by all three LIGO–Virgo detectors. The source of GW200105 has component masses 8.9+1.2-1.5 and 1.9+0.3-0.2 M⊙, whereas the source of GW200115 has component masses 5.7+1.8-2.1 and 1.5+0.7-0.3 M⊙(all measurements quoted at the 90% credible level). The probability that the secondary's mass is below the maximal mass of a neutron star is 89%–96% and 87%–98%, respectively, for GW200105 and GW200115, with the ranges arising from different astrophysical assumptions. The source luminosity distances are and 280+110-110 and 300+150-100 Mpc, respectively. The magnitude of the primary spin of GW200105 is less than 0.23 at the 90% credible level, and its orientation is unconstrained. For GW200115, the primary spin has a negative spin projection onto the orbital angular momentum at 88% probability. We are unable to constrain the spin or tidal deformation of the secondary component for either event. We infer an NSBH merger rate density of 45+75-33 Gpc-3 yr-1 when assuming that GW200105 and GW200115 are representative of the NSBH population or 130+112-69 Gpc-3 yr-1 under the assumption of a broader distribution of component masses