CO₂ transfer between the upper mantle and the atmosphere: temporary storage in the lower continental crust     

J.LR. Touret 《地学学报》1992,4(1):87-98

The CO₂ atmospheric content has shown large variations over geological times. High contents (up to one order of magnitude more than present-day values) ultimately correspond to discrete episodes of mantle degassing, either juvenile, or subduction-related (carbon recycling). A number of arguments (e.g. the continuous volume increase of carbonate-bearing sediments with time) suggest that, throughout the Earth's history, juvenile CO₂ has formed a major contribution to the global carbon budget of the Earth.
The absence of a direct relationship between major volcanic episodes and the average CO₂ atmospheric content suggests that volcanoes might not be the only way by which mantle CO₂ is transported to the surface. It is proposed that large quantities of juvenile CO₂ could temporarily be stored in the lower continental crust during major episodes of granulite formation. These are primarily caused by magmatic underplating and they result in a vertical accretion of the crust by accumulation of CO₂-bearing, mantle-derived magmas. Most of the CO₂ migrates through the crust during post-metamorphic evolution and isostatic restoration of the normal continental thickness. However, large quantities of CO₂ can still be present in some areas, notably as high-density fluids enclosed in minerals.  相似文献   

Transforming observational data and theoretical isochrones into the ACS/WFC Vega-mag system     

Luigi R. Bedin †  Santi Cassisi  Fiorella Castelli  Giampaolo Piotto  Jay Anderson  Maurizio Salaris  Yazan Momany  Adriano Pietrinferni 《Monthly notices of the Royal Astronomical Society》2005,357(3):1038-1048

We propose a zero-point photometric calibration of the data from the Advanced Camera for Surveys (ACS) Wide Field Channel (WFC) on board the Hubble Space Telescope , based on a spectrum of Vega and the most up-to-date in-flight transmission curves of the camera. This calibration is accurate at the level of a few hundredths of a magnitude. The main purpose of this effort is to transform the entire set of evolutionary models into a simple observational photometric system for ACS/WFC data, and to make them available to the astronomical community. We provide the zero-points for the most used ACS/WFC bands, and give basic recipes for calibrating both the observed data and the models. We also present the colour–magnitude diagram from ACS data of five Galactic globular clusters, spanning the metallicity range  −2.2 <[Fe/H] < −0.04  , and we provide fiducial points representing their sequences from several magnitudes below the turn-off to the red giant branch tip. The observed sequences are compared with the models in the newly defined photometric system.  相似文献   

VISTA Variables in the Via Lactea (VVV): The public ESO near-IR variability survey of the Milky Way     

D. Minniti  P.W. Lucas  J.P. Emerson  R.K. Saito  M. Hempel  P. Pietrukowicz  A.V. Ahumada  M.V. Alonso  J. Alonso-Garcia  J.I. Arias  R.M. Bandyopadhyay  R.H. Barbá  B. Barbuy  L.R. Bedin  E. Bica  J. Borissova  L. Bronfman  G. Carraro  M. Catelan  J.J. Clariá  G. Pietrzynski 《New Astronomy》2010,15(5):433-443

We describe the public ESO near-IR variability survey (VVV) scanning the Milky Way bulge and an adjacent section of the mid-plane where star formation activity is high. The survey will take 1929 h of observations with the 4-m VISTA telescope during 5 years (2010–2014), covering ～10⁹ point sources across an area of 520 deg², including 33 known globular clusters and ～350 open clusters. The final product will be a deep near-IR atlas in five passbands (0.9–2.5 μm) and a catalogue of more than 10⁶ variable point sources. Unlike single-epoch surveys that, in most cases, only produce 2-D maps, the VVV variable star survey will enable the construction of a 3-D map of the surveyed region using well-understood distance indicators such as RR Lyrae stars, and Cepheids. It will yield important information on the ages of the populations. The observations will be combined with data from MACHO, OGLE, EROS, VST, Spitzer, HST, Chandra, INTEGRAL, WISE, Fermi LAT, XMM-Newton, GAIA and ALMA for a complete understanding of the variable sources in the inner Milky Way. This public survey will provide data available to the whole community and therefore will enable further studies of the history of the Milky Way, its globular cluster evolution, and the population census of the Galactic Bulge and center, as well as the investigations of the star forming regions in the disk. The combined variable star catalogues will have important implications for theoretical investigations of pulsation properties of stars.  相似文献   

The M 4 Core Project with HST: I. Overview and first epoch     

L.R. Bedin  J. Anderson  D.C. Heggie  G. Piotto  A.P. Milone  M. Giersz  V. Nascimbeni  A. Bellini  R.M. Rich  M. van den Berg  D. Pooley  K. Brogaard  S. Ortolani  L. Malavolta  L. Ubeda  A.F. Marino 《Astronomische Nachrichten》2013,334(10):1062-1085

We present an overview of the ongoing Hubble Space Telescope large program GO‐12911. The program is focused on the core of M 4, the nearest Galactic globular cluster, and the observations are designed to constrain the number of binaries with massive companions (black holes, neutron stars, or white dwarfs) by measuring the “wobble” of the luminous (mainsequence) companion around the center of mass of the pair, with an astrometric precision of ∼50 µas. The high spatial resolution and stable medium‐band PSFs of WFC3/UVIS will make these measurements possible. In this work we describe (i) the motivation behind this study, (ii) our observing strategy, (iii) the many other investigations enabled by this unique data set, and which of those our team is conducting, and (iv) a preliminary reduction of the first‐epoch dataset collected on 2012 October 10. (© 2013 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

X‐shooter GTO observations and chemical tagging of two main‐sequence stars in the globular cluster NGC 2808     

A. Bragaglia  E. Carretta  R.G. Gratton  S. Lucatello  A. Milone  G. Piotto  V. D'Orazi  S. Cassisi  C. Sneden  R.L. Bedin 《Astronomische Nachrichten》2011,332(3):258-259

We observed two main sequence stars in the globular cluster NGC 2808, using X‐shooter. We selected one of the targets on the blue main sequence (bMS) and one on the red main sequence (rMS) and measured abundances for several light elements that are expected to be different in stars of first and second generations in globular clusters. The differences between the bMS and the rMS stars amply exceed the errors and is in agreement with a difference in products of hydrogen burning at high temperature. More data are required to put the findings on more solid basis and to try to distinguish between the different models proposed to explain the formation of globular clusters (© 2011 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

HST astrometry of the closest brown dwarfs-II. Improved parameters and constraints on a third body     

L. R. Bedin  J. Dietrich  A. J. Burgasser  D. Apai  M. Libralato  M. Griggio  C. Fontanive  D. Pourbaix 《Astronomische Nachrichten》2024,345(1):e230158

Located at less than two pc away, Luhman 16 AB (WISE J104915.57-531906.1) is the closest pair of brown dwarfs and the third closest “stellar” system to Earth. An exoplanet candidate in the Luhman 16 binary system was reported in 2017 based on a weak astrometric signature in the analysis of 12 HST epochs. An additional epoch collected in 2018 and re-analysis of the data with more advanced methods further increased the significance level of the candidate, consistent with a Neptune-mass exoplanet orbiting one of the Luhman 16 brown dwarf components. We report the joint analysis of these previous data together with two new astrometric HST epochs we obtained to confirm or disprove this astrometric signature. Our new analysis rules out the presence of a planet orbiting one component of the Luhman 16 AB system for masses $\mathrm{ℳ}$ $\gtrsim$ 1.5 M_♆ (Neptune masses) and periods between 400 and 5000 days. However, the presence of third bodies with masses $\mathrm{ℳ}$ $\lesssim$ 3 M_♆ and periods between 2 and 400 days ( $\sim$1.1 years) cannot be excluded. Our measurements make significant improvements to the characterization of this sub-stellar binary, including its mass-ratio 0.8305 $\pm 0.0006$, individual component masses 35.4 $\pm$0.2 M_Ꝝ and 29.4 $\pm$0.2 M_Ꝝ (Jupiter masses), and parallax distance 1.9960 pc $\pm$ 50 AU. Comparison of the masses and luminosities of Luhman 16 AB to several evolutionary models shows persistent discrepancies in the ages of the two components, but strengthens the case that this system is a member of the 510 $\pm$95 Myr Oceanus Moving Group.  相似文献   

Trails of solar system minor bodies on WFC/ACS images     

Simone Marchi  Yazan Momany  Luigi R. Bedin   《New Astronomy》2004,9(8):679-685

In this paper, we analyse very short arcs of minor bodies of the Solar System detected on Hubble Space Telescope (HST) Wide Field Channel ACS images. In particular, we address how to constrain the Keplerian orbital elements for minor body detections, illustrating the method for two objects. One of the minor bodies left 13 successive trails, making it the most well-sampled object yet identified in the HST archive. Most interestingly, we also address the problem of ephemeris prediction and show that in the particular case of HST very short arcs the confinement window for subsequent recovery is significantly reduced to a narrow linear region, that would facilitate successive observations.  相似文献   

应用高分辨率质谱分析苏丹高酸值原油成因   总被引：3，自引：1，他引：2  

程顶胜  窦立荣  万仑坤  史权 《岩石学报》2010,26(4):1303-1312

苏丹Muglad和Melut盆地是苏丹乃至整个中、西非剪切带最富含油气的盆地,所发现的原油主要为中质油(重度为20°～34°API),其次为重质油(重度小于20°API),普遍高含沥青质、高含蜡、高酸值、低含硫。为了探讨高酸值原油的成因,选择了苏丹地区18个不同酸值的原油样品,尝试高分辨率质谱分析上述原油有机酸的组成。结果表明,高酸值原油的有机酸主要由环烷酸组成;环烷酸的平均相对分子质量随降解作用程度增加而增大,分子碳原子数分布范围变宽;环烷酸以一环、二环、三环环烷酸为主。生物降解作用是形成高酸值原油的主要原因。  相似文献   

TASTE IV: Refining ephemeris and orbital parameters for HAT‐P‐20b and WASP‐1b     

V. Granata  V. Nascimbeni  G. Piotto  L. R. Bedin  L. Borsato  A. Cunial  M. Damasso  L. Malavolta 《Astronomische Nachrichten》2014,335(8):797-803

We present four new light curves of the transiting exoplanets WASP‐1b and HAT‐P‐20b, observed within the TASTE (The Asiago Search for Transit timing variations of Exoplanets) project. We re‐analyzed light curves from the literature in a homogeneous way, calculating a refined ephemeris and orbital‐physical parameters for both objects. WASP‐1b does not show any significant Transit Timing Variation signal at the 120 s level. As for HAT‐P‐20b, we detected a deviation from our re‐estimated linear ephemeris that could be ascribed to the presence of a perturber or, more probably, to a previously unnoticed high level of stellar activity. The rotational period of HAT‐P‐20 A that we obtained from archival data (P_rot ≃ 14.5 d), combined with its optical variability and strong emission of Ca ii H & K lines, is consistent with a young stellar age (<1 Gyr) and support the hypothesis that stellar activity may be responsible of the measured deviations of the transit times. (© 2014 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献