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M. Schwartz

Publications and source records attributed to M. Schwartz.

9 recordsLinked to original sources

An outlook on the Rapid Decline of Carbon Sequestration in French Forests and associated reporting needs

In this study, we present and discuss changes in carbon storage in the French forests from 1990 to 2022, derived from CITEPA statistics on forest carbon accounting, fed by National Forest Inventory (NFI) data collected through an extensive network of measurement sites across Metropolitan France, and other data sources as regards forest removals. The NFI is designed to provide statistical estimations of growing stock, gains and losses at the national or subnational levels but is unable, in its classical form, to provide detailed spatial outlook, such as on abrupt losses during fires, droughts and insect attacks. A continuing removal of CO2 from the atmosphere by the French forests occurred from 1990 to 2022, because harvest and mortality CO2 losses remained smaller than CO2 removals by forest growth and the increase in forest area (70,000 ha per year but insignificant in terms of increased carbon stocks at present). The CO2 removal by forests was 49.3 MtCO2 yr-1 in 1990, increased to reach a peak of 74.1 MtCO2 yr-1 in 2008 and then quickly decreased down to 37.8 Mton CO2 yr-1 in 2022. After 2017, the sink remained low and mortality rates stayed larger than during any of the previous years. This recent period is marked by climate shocks such as summer droughts and heatwaves in 2015, 2018, 2022, 2023. The full impacts of the droughts in 2022 and 2023 are not yet covered with full precision, as some of the sites measured by the national inventory before those droughts are still pending a second visit. The different regions of France show contrasted trajectories. Southern Mediterranean regions where forests have a low harvest rate have experienced a lower increase in mortality and a sustained CO2 uptake.

physics.ao-ph

3D integration and packaging for solid-state qubits

Developing a packaging scheme that meets all of the requirements for operation of solid-state qubits in a cryogenic environment can be a formidable challenge. In this article, we discuss work being done in our group as well as in the broader community, focusing on the role of 3D integration and packaging in quantum processing with solid-state qubits.

quant-ph

Diagnosing the Clumpy Protoplanetary Disk of the UXor Type Young Star GM Cephei

UX Orionis stars (UXors) are Herbig Ae/Be or T Tauri stars exhibiting sporadic occultation of stellar light by circumstellar dust. GM\,Cephei is such a UXor in the young ($\sim4$~Myr) open cluster Trumpler\,37, showing prominent infrared excess, emission-line spectra, and flare activity. Our photometric monitoring (2008--2018) detects (1)~an $\sim$3.43~day period, likely arising from rotational modulation by surface starspots, (2)~sporadic brightening on time scales of days due to accretion, (3)~irregular minor flux drops due to circumstellar dust extinction, and (4)~major flux drops, each lasting for a couple of months with a recurrence time, though not exactly periodic, of about two years. The star experiences normal reddening by large grains, i.e., redder when dimmer, but exhibits an unusual "blueing" phenomenon in that the star turns blue near brightness minima. The maximum extinction during relatively short (lasting $\leq 50$~days) events, is proportional to the duration, a consequence of varying clump sizes. For longer events, the extinction is independent of duration, suggestive of a transverse string distribution of clumps. Polarization monitoring indicates an optical polarization varying $\sim3\%$--8$\%$, with the level anticorrelated with the slow brightness change. Temporal variation of the unpolarized and polarized light sets constraints on the size and orbital distance of the circumstellar clumps in the interplay with the young star and scattering envelope. These transiting clumps are edge-on manifestations of the ring- or spiral-like structures found recently in young stars with imaging in infrared of scattered light, or in submillimeter of thermalized dust emission.

astro-ph.SR

No Transit Timing Variations in WASP-4

We present 6 new transits of the system WASP-4. Together with 28 light curves published in the literature, we perform an homogeneous study of its parameters and search for variations in the transit's central times. The final values agree with those previously reported, except for a slightly lower inclination. We find no significant long-term variations in $i$ or $R_{P}/R_{\star}$. The $O-C$ mid-transit times do not show signs of TTVs greater than 54 s.

astro-ph.EP

Early-Time Chromatic Variations in the Wind-Swept Medium of GRB 021211 and the Faintness of its Afterglow

We present Follow-Up Network for Gamma-Ray Bursts (FUN GRB) Collaboration observations of the optical afterglow of GRB 021211 made between 143 seconds and 102 days after the burst. Our unique data set includes the earliest filtered detections and color information for an afterglow in the pre-Swift era. We find that the afterglow is best described by (1) propagation through a wind-swept medium, (2) a cooling break that is blueward of the observed optical frequencies, and (3) a hard electron energy distribution. However, superimposed on this "standard model" behavior we find significant chromatic variations within the first few hours after the burst. We consider possible reasons for these variations, including the possibility that they are due to a dust echo. Finally, we constrain physical parameters that describe the afterglow and surrounding medium for a variety of scenarios and find that GRB 021211's afterglow is faint for a combination of 3-4 reasons: (1) a low fraction of energy in relativistic electrons, (2) a low density for the wind-swept medium, implying either a low mass-loss rate and/or a high wind velocity for the progenitor, (3) a wide opening/viewing angle for the jet, and possibly (4) moderate source frame extinction. The jet appears to be significantly far from equipartition and magnetically dominated. More extreme versions of this might explain the darkness of many afterglows in the Swift era.

astro-ph

Observing campaign of Eta Carinae from La Plata. Period 2003-2004

After the Observing Campaign of Eta Carinae carried out during 2003, we have continued the CCD observations using the 0.8 m Reflector telescope at La Plata Observatory, in the BVRI bands. Here, we present the results obtained since November 2003 until August 2004. In addition, we present differential photometry of other objects included in the Eta Car's frames, belonging to the open cluster Trumpler 16.

astro-ph

Optical CCD Observations of Eta Carinae at La Plata Observatory

In 2003.5 Eta Carinae was expected to undergo an X-ray eclipse (Damineli et al., 2000). In the framework of an international campaign to obtain multi-wavelength observations of this event, we have obtained optical CCD images of Eta Carinae. Here, we present the B, V, R, I, data of Eta Car obtained before and during the X-ray eclipse.

astro-ph

Stretched Exponential Decay in the Edwards-Wilkinson Model

We consider the exactly soluble Edwards-Wilkinson Model in one dimension and demonstrate explicitly, that it is possible to construct a field, that does not depend explicitly on time, such that the corresponding time dependent correlation function,, is dominated at long times by a stretched exponential decay. The difference between this and the stretched exponential decay present in truly non linear systems is discussed.

cond-mat.stat-mech

Vortex lines in the three-dimensional XY model with random phase shifts

The stability of the ordered phase of the three-dimensional XY-model with random phase shifts is studied by considering the roughening of a single stretched vortex line due to the disorder. It is shown that the vortex line may be described by a directed polymer Hamiltonian with an effective random potential that is long range correlated. A Flory argument estimates the roughness exponent to $ζ=3/4$ and the energy fluctuation exponent to $ω=1/2$, thus fulfilling the scaling relation $ω=2ζ-1$. The Schwartz-Edwards method as well as a numerical integration of the corresponding Burger's equation confirm this result. Since $ζ<1$ the ordered phase of the original XY-model is stable.

cond-mat