| 1. |
- Cedenblad, Lukas, et al.
(författare)
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Planetesimals on Eccentric Orbits Erode Rapidly
- 2021
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Ingår i: Astrophysical Journal. - : American Astronomical Society. - 0004-637X .- 1538-4357. ; 921:2
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Tidskriftsartikel (refereegranskat)abstract
- We investigate the possibility of erosion of planetesimals in a protoplanetary disk. We use theory and direct numerical simulations (lattice Boltzmann method) to calculate the erosion of large-much larger than the mean-free path of gas molecules-bodies of different shapes in flows. We find that erosion follows a universal power law in time, at intermediate times, independent of the Reynolds number of the flow and the initial shape of the body. Consequently, we estimate that planetesimals in eccentric orbits, of even very small eccentricity, rapidly (in about 100 yr) erodes away if the semimajor axis of their orbit lies in the inner disk-less than about 10 au. Even planetesimals in circular orbits erode away in approximately 10,000 yr if the semimajor axis of their orbits are <0.6 au.
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| 2. |
- Abramowicz, Marek A, 1945, et al.
(författare)
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Collisions of Neutron Stars with Primordial Black Holes as Fast Radio Bursts Engines
- 2018
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Ingår i: Astrophysical Journal. - : American Astronomical Society. - 0004-637X .- 1538-4357. ; 868:1
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Tidskriftsartikel (refereegranskat)abstract
- If primordial black holes (PBH) with masses of 10(25) g greater than or similar to m greater than or similar to 10(17) g constitute a non-negligible fraction of galactic dark-matter halos, their existence should have observable consequences: they necessarily collide with galactic neutron stars (NS), nest in their centers, and accrete the dense matter, eventually converting them to NS-mass black holes while releasing the NS magnetic field energy. Such processes may explain the fast radio bursts (FRB) phenomenology, in particular their millisecond durations, large luminosities similar to 10(43) erg s(-1), high rate of occurrence greater than or similar to 1000 day(-1), as well as high brightness temperatures, polarized emission, and Faraday rotation. Longer than the dynamical timescale of the Bondi-like accretion for light PBH allows for the repeating of FRB. This explanation follows naturally from the (assumed) existence of the dark-matter PBH and requires no additional unusual phenomena, in particular no unacceptably large magnetic fields of NS. In our model, the observed rate of FRB throughout the universe follows from the presently known number of NS in the Galaxy.
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| 3. |
- Gorai, Prasanta, 1991, et al.
(författare)
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Astrochemical Diagnostics of the Isolated Massive Protostar G28.20-0.05
- 2024
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Ingår i: Astrophysical Journal. - 1538-4357 .- 0004-637X. ; 960:2
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Tidskriftsartikel (refereegranskat)abstract
- We study the astrochemical diagnostics of the isolated massive protostar G28.20-0.05. We analyze data from Atacama Large Millimeter/submillimeter Array 1.3 mm observations with a resolution of 0.″2 (∼1000 au). We detect emission from a wealth of species, including oxygen-bearing (e.g., H2CO, CH3OH, CH3OCH3), sulfur-bearing (SO2, H2S), and nitrogen-bearing (e.g., HNCO, NH2CHO, C2H3CN, C2H5CN) molecules. We discuss their spatial distributions, physical conditions, correlation between different species, and possible chemical origins. In the central region near the protostar, we identify three hot molecular cores (HMCs). HMC1 is part of a millimeter continuum ring-like structure, is closest in projection to the protostar, has the highest temperature of ∼300 K, and shows the most line-rich spectra. HMC2 is on the other side of the ring, has a temperature of ∼250 K, and is of intermediate chemical complexity. HMC3 is further away, ∼3000 au in projection, cooler (∼70 K), and is the least line-rich. The three HMCs have similar mass surface densities (∼10 g cm−2), number densities (n H ∼ 109 cm−3), and masses of a few solar masses. The total gas mass in the cores and in the region out to 3000 au is ∼25 M ⊙, which is comparable to that of the central protostar. Based on spatial distributions of peak line intensities as a function of excitation energy, we infer that the HMCs are externally heated by the protostar. We estimate column densities and abundances of the detected species and discuss the implications for hot core astrochemistry.
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| 4. |
- Holmlid, Leif, 1942
(författare)
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Ultradense Hydrogen H(0) as Stable Dark Matter in the Universe: Extended Red Emission Spectra Agree with Rotational Transitions in H(0)
- 2018
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Ingår i: Astrophysical Journal. - : American Astronomical Society. - 0004-637X .- 1538-4357. ; 866:2
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Tidskriftsartikel (refereegranskat)abstract
- Studies of ultradense hydrogen H(0) in our laboratory have been reported in around 50 publications. The proton solar wind was shown to agree well with the protons ejected by Coulomb explosions in p(0). H(0) is a quantum material and can have at least two slightly different forms-ultradense protium p(0) and ultradense deuterium D(0)-which are stable even inside many stars. Mixed phases pD(0) have also been studied. These phases are the lowest-energy forms of hydrogen, and H(0) will probably exist everywhere where hydrogen exists in the universe. Rotational spectra from H(0) have been studied in laboratory experiments in emission in the visible range, giving good agreement with observations of ERE (extended red emission) in space. The ERE bands and sharp peaks agree with rotational transitions for a few coupled p-p and p-D pairs in the well studied spin state s - 4 in H(0). Since ERE is observed almost everywhere in space, this proves that H(0) is common in space. The rotational absorption from the ground state in p(0) agrees with the 220 nm extinction bump for three coupled p-p pairs in the most common spin state s - 2 studied. The uneven distribution of deuterium in space may be due to the slightly different properties of D(0), which separate it from p(0). The dark "missing mass" concluded to exist in the halos of rotating galaxies is proposed as being due to accumulation of H(0) there. Other important implications of the superfluid and superconductive phase H(0) in space await discovery.
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| 5. |
- Liu, F. K., et al.
(författare)
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Elliptical Accretion Disk as a Model for Tidal Disruption Events
- 2021
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Ingår i: Astrophysical Journal. - : American Astronomical Society. - 0004-637X .- 1538-4357. ; 908:2
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Tidskriftsartikel (refereegranskat)abstract
- Elliptical accretion disk models for tidal disruption events (TDEs) have been recently proposed and independently developed by two groups. Although these two models are characterized by a similar geometry, their physical properties differ considerably. In this paper, we further investigate the properties of the elliptical accretion disk of the nearly uniform distribution of eccentricity within the disk plane. Our results show that the elliptical accretion disks have distinctive hydrodynamic structures and spectral energy distributions, associated with TDEs. The soft X-ray photons generated at pericenter and nearby are trapped in the disk and advected around the ellipse because of large electron scattering opacity. They are absorbed and reprocessed into emission lines and low-frequency continuum via recombination and bremsstrahlung emission. Because of the rapid increase of bound-free and free-free opacities with radius, the low-frequency continuum photons become trapped in the disk at large radius and are advected through apocenter and back to the photon-trapping radius. Elliptical accretion disks predict sub-Eddington luminosities and emit mainly at the photon-trapping radius of thousands of Schwarzschild radii with a blackbody spectrum of nearly single temperature of typically about 3 x 10(4) K. Because of the self-regulation, the photon-trapping radius expands and contracts following the rise and fall of accretion rate. The radiation temperature is nearly independent of BH mass and accretion rate and varies weakly with the stellar mass and the viscosity parameter. Our results are well consistent with the observations of optical/UV TDEs.
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| 6. |
- Mulders, G. D., et al.
(författare)
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Constraints from Dust Mass and Mass Accretion Rate Measurements on Angular Momentum Transport in Protoplanetary Disks
- 2017
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Ingår i: Astrophysical Journal. - : American Astronomical Society. - 0004-637X .- 1538-4357. ; 847:1
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Tidskriftsartikel (refereegranskat)abstract
- In this paper, we investigate the relation between disk mass and mass accretion rate to constrain the mechanism of angular momentum transport in protoplanetary disks. We find a correlation between dust disk mass and mass accretion rate in Chamaeleon I with a slope that is close to linear, similar to the one recently identified in Lupus. We investigate the effect of stellar mass and find that the intrinsic scatter around the best-fit M-dust-M star and M-acc-M star relations is uncorrelated. We simulate synthetic observations of an ensemble of evolving disks using a Monte Carlo approach and find that disks with a constant alpha viscosity can fit the observed relations between dust mass, mass accretion rate, and stellar mass but overpredict the strength of the correlation between disk mass and mass accretion rate when using standard initial conditions. We find two possible solutions. In the first one, the observed scatter in M-dust and M-acc is not primordial, but arises from additional physical processes or uncertainties in estimating the disk gas mass. Most likely grain growth and radial drift affect the observable dust mass, while variability on large timescales affects the mass accretion rates. In the second scenario, the observed scatter is primordial, but disks have not evolved substantially at the age of Lupus and Chamaeleon I owing to a low viscosity or a large initial disk radius. More accurate estimates of the disk mass and gas disk sizes in a large sample of protoplanetary disks, through either direct observations of the gas or spatially resolved multiwavelength observations of the dust with ALMA, are needed to discriminate between both scenarios or to constrain alternative angular momentum transport mechanisms such as MHD disk winds.
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| 7. |
- Radhakrishnan, Soumya, et al.
(författare)
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Photochemical Processes in CO2/H2O Ice Mixtures with Trapped Pyrene, a Model Polycyclic Aromatic Hydrocarbon
- 2018
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Ingår i: Astrophysical Journal. - : American Astronomical Society. - 0004-637X .- 1538-4357. ; 864:2
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Tidskriftsartikel (refereegranskat)abstract
- Vacuum ultraviolet irradiation of a polycyclic aromatic hydrocarbon molecule, pyrene, trapped in carbon dioxide (CO2)-enriched astrophysical ice analogues has been studied and presented here. Pyrene is co-deposited with a gaseous mixture of H2O and CO2 (100% CO2; 50:50 CO2:H2O; and 100% H2O) and is subjected to Lye, photons from a hydrogen-flow microwave discharge lamp. To our surprise, we found ionization of pyrene in all three ices, with ionization yields following the H2O content in the ice, indicating that H2O ice stabilizes charged ions and electrons better than CO2 ice by a factor of 10. Caution needs to be exercised not to overinterpret our finding that pyrene is ionized in pure CO2 ice, because even trace amounts of water in the CO2 matrix could result in an increased ionization of pyrene. In addition to ionization of pyrene in CO2 ice, photochemical products of the CO2 ice itself, namely CO and CO3, were found to form efficiently, as detected using Fourier transform infrared spectroscopy, in agreement with earlier studies. UV vis spectra showed formation of ozone (O-3) with prolonged irradiation. Surprisingly, O-3 yields followed CO2 concentration in the ice mixtures, with the strongest bands in photolyzed CO2 ice and the weakest in photolyzed H2O ice, indicating that CO2 ice is very protoreactive and produces more O atoms than H2O ice. Pyrene-containing photoproducts, incorporating CO2 or CO or O, such as Py-COOH, Py-OH, or Py-CHO, are not explicitly seen in the UV vis absorption spectra, but we cannot rule out the possibility that their UV absorption may be swamped under the strong absorption of O-3.
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| 8. |
- Abramowicz, Marek A, 1945, et al.
(författare)
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No Observational Constraints from Hypothetical Collisions of Hypothetical Dark Halo Primordial Black Holes with Galactic Objects
- 2009
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Ingår i: Astrophysical Journal. - 0004-637X .- 1538-4357. ; 705:1, s. 659-669
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Tidskriftsartikel (refereegranskat)abstract
- It was suggested by several authors that hypothetical primordial black holes (PBHs) may contribute to the dark matter (DM) in our Galaxy. There are strong constraints based on the Hawking evaporation that practically exclude PBHs with masses m pbh ~ 1015to1016 g and smaller as significant contributors to the Galactic DM. Similarly, PBHs with masses greater than about 1026 g are practically excluded by the gravitational lensing observation. The mass range between 1016 g
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| 9. |
- Pascucci, I., et al.
(författare)
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A steeper than linear disk mass-stellar mass scaling relation
- 2016
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Ingår i: Astrophysical Journal. - 0004-637X .- 1538-4357. ; 831
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Tidskriftsartikel (refereegranskat)abstract
- © 2016. The American Astronomical Society. All rights reserved. The disk mass is among the most important input parameter for every planet formation model to determine the number and masses of the planets that can form. We present an ALMA 887 μm survey of the disk population around objects from ∼2 to 0.03 M o in the nearby ∼2 Myr old Chamaeleon I star-forming region. We detect thermal dust emission from 66 out of 93 disks, spatially resolve 34 of them, and identify two disks with large dust cavities of about 45 au in radius. Assuming isothermal and optically thin emission, we convert the 887 μm flux densities into dust disk masses, hereafter M dust. We find that the relation is steeper than linear and of the form M dust ∝ (M ∗)1.3-1.9, where the range in the power-law index reflects two extremes of the possible relation between the average dust temperature and stellar luminosity. By reanalyzing all millimeter data available for nearby regions in a self-consistent way, we show that the 1-3 Myr old regions of Taurus, Lupus, and Chamaeleon I share the same relation, while the 10 Myr old Upper Sco association has a steeper relation. Theoretical models of grain growth, drift, and fragmentation reproduce this trend and suggest that disks are in the fragmentation-limited regime. In this regime millimeter grains will be located closer in around lower-mass stars, a prediction that can be tested with deeper and higher spatial resolution ALMA observations.
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| 10. |
- Svoboda, B. E., et al.
(författare)
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THE BOLOCAM GALACTIC PLANE SURVEY. XIV. PHYSICAL PROPERTIES of MASSIVE STARLESS and STAR-FORMING CLUMPS
- 2016
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Ingår i: Astrophysical Journal. - 0004-637X .- 1538-4357. ; 822:2
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Tidskriftsartikel (refereegranskat)abstract
- We sort 4683 molecular clouds between 10° < ℓ < 65° from the Bolocam Galactic Plane Survey based on observational diagnostics of star formation activity: compact 70 μm sources, mid-IR color-selected YSOs, H2O and CH3OH masers, and UCH ii regions. We also present a combined NH3-derived gas kinetic temperature and H2O maser catalog for 1788 clumps from our own GBT 100 m observations and from the literature. We identify a subsample of 2223 (47.5%) starless clump candidates (SCCs), the largest and most robust sample identified from a blind survey to date. Distributions of flux density, flux concentration, solid angle, kinetic temperature, column density, radius, and mass show strong (>1 dex) progressions when sorted by star formation indicator. The median SCC is marginally subvirial (α ∼ 0.7) with >75% of clumps with known distance being gravitationally bound (α < 2). These samples show a statistically significant increase in the median clump mass of ΔM ∼ 170-370 M o from the starless candidates to clumps associated with protostars. This trend could be due to (i) mass growth of the clumps at M o Myr-1 for an average freefall 0.8 Myr timescale, (ii) a systematic factor of two increase in dust opacity from starless to protostellar phases, and/or (iii) a variation in the ratio of starless to protostellar clump lifetime that scales as ∼M -0.4. By comparing to the observed number of CH3OH maser containing clumps, we estimate the phase lifetime of massive (M > 103 M o) starless clumps to be 0.37 ± 0.08 Myr (M/103 M o)-1; the majority (M < 450 M o) have phase lifetimes longer than their average freefall time. © 2016. The American Astronomical Society. All rights reserved.
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