1,146 research outputs found
Analysis and test of the central-blue-spot infall hallmark
The infall of material onto a protostar, in the case of optically thick line
emission, produces an asymmetry in the blue- and red-wing line emission. For an
angularly resolved emission, this translates in a blue central spot in the
first-order moment (intensity weighted velocity) map. An analytical expression
for the first-order moment intensity as a function of the projected distance
was derived, for the cases of infinite and finite infall radius. The effect of
a finite angular resolution, which requires the numerical convolution with the
beam, was also studied. This method was applied to existing data of several
star-forming regions, namely G31.41+0.31 HMC, B335, and LDN 1287, obtaining
good fits to the first-order moment intensity maps, and deriving values of the
central masses onto which the infall is taking place (G31.41+0.31 HMC: 70-120
; B335: 0.1 ; Guitar Core of LDN 1287: 4.8 ). The
central-blue-spot infall hallmark appears to be a robust and reliable indicator
of infall.Comment: Accepted for publication in A&
High-cadence spectroscopy of M-dwarfs – II. Searching for stellar pulsations with HARPS
Stellar oscillations appear all across the Hertzsprung–Russell diagram. Recent theoretical studies support their existence also in the atmosphere of M dwarfs. These studies predict for them short periodicities ranging from 20 min to 3 h. Our Cool Tiny Beats (CTB) programme aims at finding these oscillations for the very first time. With this goal, CTB explores the short time domain of M dwarfs using radial velocity data from the High Accuracy Radial velocity Planet Searcher (HARPS)-European Southern Observatory and HARPS-N high-precision spectrographs. Here we present the results for the two most long-term stable targets observed to date with CTB, GJ 588 and GJ 699 (i.e. Barnard's star). In the first part of this work we detail the correction of several instrumental effects. These corrections are especially relevant when searching for subnight signals. Results show no significant signals in the range where M dwarfs pulsations were predicted. However, we estimate that stellar pulsations with amplitudes larger than ∼0.5 m s−1 can be detected with a 90 per cent completeness with our observations. This result, along with the excess of power regions detected in the periodograms, opens the possibility of non-resolved very low amplitude pulsation signals. Next generation more precise instrumentation would be required to detect such oscillations. However, the possibility of detecting pulsating M-dwarf stars with larger amplitudes is feasible due to the short size of the analysed sample. This motivates the need for completeness of the CTB survey
The L723 low mass star forming protostellar system: resolving a double core
We present 1.35 mm SMA observations around the low-mass Class 0 source IRAS
19156+1906, at the the center of the L723 dark cloud. We detected emission from
dust as well as emission from H2CO, DCN and CN, which arise from two cores, SMA
1 and SMA 2, separated by 2.9" (880 AU). SMA 2 is associated with VLA 2. SiO
5-4 emission is detected, possibly tracing a region of interaction between the
dense envelope and the outflow. We modeled the dust and the H2CO emission from
the two cores: they have similar physical properties but SMA 2 has a larger
p-H2CO abundance than SMA 1. The p-H2CO abundances found are compatible with
the value of the outer part of the circumstellar envelopes associated with
Class 0 sources. SMA 2 is likely more evolved than SMA 1. The kinematics of the
two sources show marginal evidence of infall and rotation motions. The mass
detected by the SMA observation, which trace scales of ~1000 AU, is only a
small fraction of the mass contained in the large scale molecular envelope,
which suggests that L723 is still in a very early phase of star formation.
Despite the apparent quiescent nature of the L723, fragmentation is occurring
at the center of the cloud at different scales. Thus, at 1000 AU the cloud has
fragmented in two cores, SMA 1 and SMA 2. At the same time, at least one of
these cores, SMA 2, has undergone additional fragmentation at scales of 150 AU,
forming a multiple stellar system.Comment: 35 pages, 15 figures. Accepted to the Astrophysical Journa
Statistical Analysis of Water Masers in Star-Forming Regions: Cepheus A and W75 N
We have done a statistical analysis of Very Long Baseline Array (VLBA) data
of water masers in the star-forming regions (SFRs) Cepheus A and W75 N, using
correlation functions to study the spatial clustering and Doppler-velocity
distribution of these masers. Two-point spatial correlation functions show a
characteristic scale size for clusters of water maser spots < or ~1 AU, similar
to the values found in other SFRs. This suggests that the scale for water maser
excitation tends to be < or ~1 AU. Velocity correlation functions show
power-law dependences with indices that can be explained by regular velocity
fields, such as expansion and/or rotation. These velocity fields are similar to
those indicated by the water maser proper-motion measurements; therefore, the
velocity correlation functions appear to reveal the organized motion of water
maser spots on scales larger than 1 AU.Comment: 16 pages, 8 figures, and 3 tables. Accepted by The Astrophysical
Journa
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