Andira Rosa | University of Esa Unggul (original) (raw)
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Papers by Andira Rosa
New Forests, 2011
Secondary successional vegetation represents one-third of the 7% of the original area covered wit... more Secondary successional vegetation represents one-third of the 7% of the original area covered with tropical dry forest that remains in central Veracruz, Mexico. In this region, fallow periods are short, in general, no longer than 7–10 years, and old secondary successional sites are not available. Therefore we evaluated the potential of very early successional stages of tropical dry forest with different land use histories for recovering the structure and composition of regional forest. We compared five early successional sites (7–72 months) with five nearby forest remnants. Successional sites had reached 38 and 30%, respectively, of the average basal area and density recorded for the forest understories, but only 5 and 10%, respectively, of the basal area and density of forest overstories. A total of 132 tree species were recorded, 45 at successional and 107 at forest sites. Individuals of tree species with animal-dispersed seeds (57%) were significantly better represented than wind-dispersed (22%) and self-dispersing (21%) species in both successional and forest sites. Successional sites had already recruited 10% of the intermediate and shade-tolerant species that grow in forest remnants. However, only 20 species occurred in both early successional and forest sites, several showing resprouting ability. We conclude that the entry of forest species to the successional process at very early stages and the recruitment of individuals from resprouting may facilitate the recovery of the dry forest in Veracruz.
Astronomy & Astrophysics, 2011
We construct an all-sky map of the apparent temperature and optical depth of thermal dust emissio... more We construct an all-sky map of the apparent temperature and optical depth of thermal dust emission using the Planck-HFI and IRAS data. The optical depth maps are correlated to tracers of the atomic and molecular gas. The correlation is linear in the lowest column density regions at high galactic latitudes. At high NH, the correlation is consistent with that of the lowest NH. In the intermediate NH range, we observe departure from linearity, with the dust optical depth in excess to the correlation. We attribute this excess emission to thermal emission by dust associated with a Dark-Gas phase, undetected in the available HI and CO measurements. We show the 2D spatial distribution of the Dark-Gas in the solar neighborhood and show that it extends around known molecular regions traced by CO. The average dust emissivity in the HI phase in the solar neighborhood follows roughly a power law distribution with beta = 1.8 all the way down to 3 mm, although the SED flattens slightly in the millimetre. The threshold for the existence of the Dark-Gas is found at NH = (8.0\pm 0.58) 10^{20} Hcm-2. Assuming the same dust emissivity at high frequencies for the dust in the atomic and molecular phases leads to an average XCO = (2.54\pm0.13) 10^{20} H2cm-2/(K km s-1). The mass of Dark-Gas is found to be 28% of the atomic gas and 118% of the CO emitting gas in the solar neighborhood. A possible origin for the Dark-Gas is the existence of a dark molecular phase, where H2 survives photodissociation but CO does not. The observed transition for the onset of this phase in the solar neighborhood (AV = 0.4 mag) appears consistent with recent theoretical predictions. We also discuss the possibility that up to half of the Dark-Gas could be in atomic form, due to optical depth effects in the HI measurements.
New Forests, 2011
Secondary successional vegetation represents one-third of the 7% of the original area covered wit... more Secondary successional vegetation represents one-third of the 7% of the original area covered with tropical dry forest that remains in central Veracruz, Mexico. In this region, fallow periods are short, in general, no longer than 7–10 years, and old secondary successional sites are not available. Therefore we evaluated the potential of very early successional stages of tropical dry forest with different land use histories for recovering the structure and composition of regional forest. We compared five early successional sites (7–72 months) with five nearby forest remnants. Successional sites had reached 38 and 30%, respectively, of the average basal area and density recorded for the forest understories, but only 5 and 10%, respectively, of the basal area and density of forest overstories. A total of 132 tree species were recorded, 45 at successional and 107 at forest sites. Individuals of tree species with animal-dispersed seeds (57%) were significantly better represented than wind-dispersed (22%) and self-dispersing (21%) species in both successional and forest sites. Successional sites had already recruited 10% of the intermediate and shade-tolerant species that grow in forest remnants. However, only 20 species occurred in both early successional and forest sites, several showing resprouting ability. We conclude that the entry of forest species to the successional process at very early stages and the recruitment of individuals from resprouting may facilitate the recovery of the dry forest in Veracruz.
Astronomy & Astrophysics, 2011
We construct an all-sky map of the apparent temperature and optical depth of thermal dust emissio... more We construct an all-sky map of the apparent temperature and optical depth of thermal dust emission using the Planck-HFI and IRAS data. The optical depth maps are correlated to tracers of the atomic and molecular gas. The correlation is linear in the lowest column density regions at high galactic latitudes. At high NH, the correlation is consistent with that of the lowest NH. In the intermediate NH range, we observe departure from linearity, with the dust optical depth in excess to the correlation. We attribute this excess emission to thermal emission by dust associated with a Dark-Gas phase, undetected in the available HI and CO measurements. We show the 2D spatial distribution of the Dark-Gas in the solar neighborhood and show that it extends around known molecular regions traced by CO. The average dust emissivity in the HI phase in the solar neighborhood follows roughly a power law distribution with beta = 1.8 all the way down to 3 mm, although the SED flattens slightly in the millimetre. The threshold for the existence of the Dark-Gas is found at NH = (8.0\pm 0.58) 10^{20} Hcm-2. Assuming the same dust emissivity at high frequencies for the dust in the atomic and molecular phases leads to an average XCO = (2.54\pm0.13) 10^{20} H2cm-2/(K km s-1). The mass of Dark-Gas is found to be 28% of the atomic gas and 118% of the CO emitting gas in the solar neighborhood. A possible origin for the Dark-Gas is the existence of a dark molecular phase, where H2 survives photodissociation but CO does not. The observed transition for the onset of this phase in the solar neighborhood (AV = 0.4 mag) appears consistent with recent theoretical predictions. We also discuss the possibility that up to half of the Dark-Gas could be in atomic form, due to optical depth effects in the HI measurements.