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Angiopteris nodosipetiolata Ting Wang tris, H.F.Chen & Y.H.Yan, a new fern of Marattiaceae, is described and illustrated. Morphologically, A. nodosipetiolata is similar to A. chingii with more than one naked pulvinus on the stipe and numerous jointed hairs on the undersides of the mature pinnae. However, the pinnae of A. nodosipetiolata are lanceolate and can reach up to 4–6 pairs, whereas they are elliptic and occur in 2–3 pairs in A. chingii. Phylogenetic and genetic distance analysis, based on the plastid genomes, also indicates that A. nodosipetiolata is not closely related to A. chingii. Currently, there are ca. 500 mature individuals in Gulinqing Nature Reserve and we suggest A. nodosipetiolata should be categorised as an Endangered (EN) species according to the criteria of IUCN. [ABSTRACT FROM AUTHOR]

Two new species of Christisonia (Orobanchaceae), Christisonia hekouensis Gui L.Zhang, J.D.Ya & W.B.Yu and Christisonia dentosa J.D.Ya, Gui L.Zhang & W.B.Yu, found during botanical surveys in Southeast Yunnan, China, are described and illustrated. The two new species are similar to C. kwangtungensis bearing rose-red flowers and conspicuously inflated corolla tubes, and phylogenetic analyses strongly support the three species as monophyletic. However, C. hekouensis can be distinguished from C. kwangtungensis and C. dentosa by having externally puberulent calyces and corollas, corolla lobes with serrulate margins, styles that are pink and glabrous or sparsely capitate-glandular pubescent above, and with anthers less than 2 mm below the stigma. Christisonia dentosa differs from C. kwangtungensis and C. hekouensis by having dentate corolla lobe margins, internally capitate-glandular pubescent corollas, styles distinctly capitate-glandular pubescent above, and more than six anthers which are up to 10 mm below the stigma. [ABSTRACT FROM AUTHOR]

Impatiens spiralis, a new species of Balsaminaceae from Hekou County, Yunnan, China, is described and illustrated. This new species is similar to I. hongkongensis, but differs in its obovate‐lanceolate or oblong lamina, without glands at base, spirally curved spur and dorsal petal suborbicular or oblate. Moreover, a phylogenetic analysis based on nuclear ITS and plastid atpB‐rbcL suggests that the new species should be placed in I. subg. Clavicarpa. [ABSTRACT FROM AUTHOR]

In 2019 January, the appearance of asteroid 6478 Gault immediately attracted attention because this object exhibited a long and thin tail that was quite different from the usual asteroids. This unexpected morphology placed asteroid 6478 Gault into the catalogue of active asteroids. We acquired photometric and spectroscopic observations on 37 nights from 2019 January to April using several telescopes, including LOT (1 m telescope) and SLT (40 cm telescope) at Lulin Observatory, and the 2.4 m telescope at Lijiang station of Yunnan Observatory. We did not find any reliable value for the rotational period of Gault during 2.5 hr and 5 hr observations on 2019 January 26 at Lijiang station and March 25 at Lulin Observatory, respectively. We classified 6478 Gault as a Q-type asteroid using visible spectrum and photometric measurements, including colors (B − V avg = 0.764 ± 0.045, V − R avg = 0.450 ± 0.023), and relative reflectance. By using Finson–Probstein analysis, the grain size for Gault's tail 2 is larger than 20 μm. [ABSTRACT FROM AUTHOR]

Abstract: The mutual eclipse of S4 Dione by S3 Tethys (Dec 23, 2009) and mutual occultation of S3 Tethys by S4 Dione (Apr 24, 2010) were observed at Yunnan Observatory during the international campaign in 2009–2010. The aim of this paper is to calculate the astrometric data of the involved Saturnian satellites during the mutual events, using a same dynamical model as proposed by Assafin et al. (2009) for the mutual occultation and a same one as proposed by Zhang and Liu (2011) for the mutual eclipse, and taking the scattering properties of the Saturnian satellites surfaces into account. Compared with the theory TASS 1.7 (Vienne and Duriez, 1995), the O–C(x) and O–C(y) are 10.1mas, 3.4mas for the mutual eclipse S4 by S3 and 28.4mas, −1.3mas for the mutual occultation S3 by S4, and with respect to the theory by Lainey et al. (2011), the results are 1.0mas, −5.0mas and −0.2mas, 2.5mas respectively. [Copyright &y& Elsevier]