Parasitism of horsehair worm in mantids were investigated for two years, from 2012 and 2013. The mantids were collected from forty-nine sites from August to November. Twenty-one sites (42.9%) of the collected mantids were parasitized by horsehair worms. C. japonensis was recorded from T. angustipennis, T. aridifolia and C. fukuii. The C. japonensis parasitism of T. angustipennis and T. aridifolia were 27.0% and 10.7%, respectively. The infested number of C. japonensis was 1-9 per host. The body length of C. japonensis showed tendency to decrease with number of parasites, but not significantly different. Horsehair worms did not affect body, abdomen length and digestive system of host. However, egg possession of host was different, unparasitized T. angustipennis and T. aridifolia had more eggs (63.7%) than parasitized ones (2.6%). C. japonensis was parasitized as immature stage in late Aug. immature and adult stage in early Sept. and only adult in late Oct. Parasitism was the highest in late Sept.

The the peach pyralid moth, Dichocrocis punctiferalis causes the most serious damage to chestnut in Korea. This study was conducted to compare the efficiency of control with aerial spraying(AS350-B2 Helicopter, 15m/flight altitude, Nozzleorifice D6, Fenitrothion EC 50% 1ℓ/ha), sex pheromone trap(25 Wing traps/ha, 75:25 mixture of (E)-10-hexadecenyl aldehyde (E10-16:Al) and (Z)-10-hexadecenyl aldehyde, 1㎎/trap), and crown spraying(BF530, Fenitrothion EC 50% 1ℓ/ha) against D. punctiferalis at chestnut orchards. After chestnut harvest in Autumn, the damaged rate(%) by D. punctiferalis showed 29.6±1.7 in aerial spraying, 27.8±8.4 in sex pheromone trap, and 8.9±3.8 in crown spraying, respectively. The crown spraying showed the highest control effect among the 3 control methods. The other methods were similarly effective.

We present UBVRI CCD photometry of the Type Ie supernova SN 19941 in M51 which was discovered on April 2, 1994 (UT). UBVRI CCD photometry of SN 1994 I were obtained for the period of the first two months from April 4, 1994, using the Seoul National University Observatory 60 cm telescope. The light curves of SN 19941 show several interesting features: (a) SN 19941 reaches the maximum brightness at B-band on April 8.23 (B = 13.68 mag), at V-band on April 9.10 (V = 12.89 mag), and at I-band on April 10.32 (I = 12.48 mag); (b) The light curves around the maximum brightness are much narrower than those of other types of supernovae; (c) The light curves after the peak decline more steeply than those of other types of supernovae; and (d) The colors get redder from (V-R) ≈ 0.2 mag ((V - I) ≈ 0.3 mag, (B - V) ≈ 0.7 mag) on April 4 to (V-R)≈ 0.6 mag ((V-1) ≈0.9 mag, (B-V) ≈ 1.3 mag) on April 18. Afterwards (V - R) colors get bluer slightly (by ~0.005 mag/day), while (V-I) colors stay almost constant around (V-1) ≈ 1.0 mag. The color at the maximum brightness is (B-V)=0.9 mag, which is ~1 mag redder than the mean color of typical Type la supernovae at the maximum brightness. The light curves of SN 1994I are similar to those of the Type Ie supernova SN 1962L in NGC 1073. Adopting the distance modulus of (m-M)0 = 29.2 mag and the reddening of E(B - V) = 0.45 mag [Iwamoto et al. 1994, preprint for ApJ], we derive absolute magnitudes at the maximum brightness of SN 1994I, Mv(max) = -17.7 mag and MB(max) = -17.4 mag. This result shows that SN 1994I was ~2 mag fainter at the maximum brightness compared with typical Type Ia supernovae. A narrower peak and faster decline after the maximum in the light curve of SN 1994I compared with other types of supernovae indicate that the progenitor of SN 1994I might be a lower mass star compared with those of other types of supernovae.