Prediction for national catastrophe fund     

Pushkar Aggarwal 《Natural Hazards》2012,60(2):263-271

United States of America (US) Congress is considering a bill ‘H.R. 2555: Homeowners’ Defense Act of 2010’ to form National Catastrophe Risk Consortium, one of whose functions is to fund a National Catastrophe Fund to help public and insurance companies meet the liability claims from hurricane, fire, and blizzard. However, before the act is enacted into law by US Congress, the bill has to pass through House Financial Services Committee which takes into account the projected costs, disbursements, and the amount required to be appropriated for the task and its source. Using data for three catastrophes for the last 100 years, the 2011 claims for hurricane, fire, and blizzard in United States of America are estimated. For predicting acres burned and economic damage due to blizzards, a trend analysis and linear regression were carried out using Excel and GraphPad Prism. Poisson distribution was used to model hurricanes. The estimates for the different catastrophes are based on a 95% confidence interval. The cost to the National Catastrophe Fund for the liabilities of fire, blizzard, and hurricane comes to over 2 billion. Of this, the bulk cost arises from fire damage, followed by hurricane damage and blizzard damage.  相似文献   

[Al ii] in the ultraviolet spectrum of the symbiotic star RR Telescopii     

F. P. Keenan  B. R. Espey  M. Mathioudakis  K. M. Aggarwal  F. L. Crawford  W. A. Feibelman  F. C. McKenna 《Monthly notices of the Royal Astronomical Society》1999,309(1):195-198

An inspection of a GHRS/ HST spectrum of the symbiotic star RR Telescopii reveals the presence of the [Al  ii ] 3s²¹S – 3s3p ³P₂ line at a vacuum wavelength of 2661.06±0.08 Å, 8.89±0.08 Å away from the Al  ii ] 3s²¹S – 3s3p ³P₁ intercombination transition at 2669.95 Å, in good agreement with the theoretical prediction of Δ λ =8.80 Å. We also find that the Al  ii ] line profile is asymmetric, showing a strong low-density component with a weak high-density wing, redshifted by 30 km s⁻¹, in agreement with the findings of Schild & Schmid, which were based on optical observations. Our measurement of the emission-line ratio R I (2661.06 Å)/ I (2669.95 Å)=0.027±0.003 implies log  N _e=5.8±0.2, in good agreement with the densities found from other ions, such as Si  iii . These results provide strong evidence that we have detected the [Al  ii ] line, the first time (to our knowledge) that this feature has been reliably identified in an astrophysical or laboratory spectrum.  相似文献   

Stabilization characteristics of copper mine tailings through its utilization as a partial substitute for cement in concrete: preliminary investigations     

Sanghamitra Kundu  Aman Aggarwal  Siddharth Mazumdar  K. Bhargava Dutt 《Environmental Earth Sciences》2016,75(3):227

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Estimation of structural vulnerability for flooding using geospatial tools in the rural area of Orissa,India     

Praveen K. Thakur  Sreyasi Maiti  Nanette C. Kingma  V. Hari Prasad  S. P. Aggarwal  Ashutosh Bhardwaj 《Natural Hazards》2012,61(2):501-520

Vulnerability assessment of natural disasters is a crucial input for risk assessment and management. In the light of increasing frequency of disasters, societies must become more disaster resilient. This research tries to contribute to this aim. For risk assessment, insight is needed into the hazard, the elements at risk and their vulnerabilities. This study focused on the estimation of structural vulnerability due to flood for a number of structural elements at risk in the rural area of Orissa, India (Kendrapara), using a community-based approach together with geospatial analysis tools. Sixty-three households were interviewed about the 2003 floods in 11 villages and 166 elements at risk (buildings) were identified. Two main structural types were identified in the study area, and their vulnerability curves were made by plotting the relationships between flood depth and vulnerability for each structural type. The vulnerability ranges from 0 (no damage) to 1 (collapse/total damage). Structural type-1 is characterized by mud wall/floor material and a roof of paddy straw, and structural type-2 is characterized by reinforced cement concrete (RCC) walls/floor and a RCC roof. The results indicate that structural type-1 is most vulnerable for flooding. Besides flood depth, flood duration is also of major importance. Houses from structural type-1 were totally collapsed after 3 days of inundation. Damage of the houses of structural type-2 began after 10 days of inundation.  相似文献   

Relationship between CME dynamics and solar flare plasma     

Rajmal Jain  Malini Aggarwal  Pradeep Kulkarni 《中国天文和天体物理学报》2010,10(5)

The relationship between the velocity of CMEs and the plasma temperature of the associated X-ray solar flares is investigated.The velocity of CMEs increases with plasma temperature(R=0.82)and photon index below the break energy(R=0.60)of X-ray flares.The heating of the coronal plasma appears to be significant with respect to the kinetics of a CME from the reconnection region where the flare also occurs.We propose that the initiation and velocity of CMEs perhaps depend upon the dominant process of conversion of the magnetic field energy of the active region to heating/accelerating the coronal plasma in the reconnected loops.Results show that a flare and the associated CME are two components of one energy release system,perhaps,magnetic field free energy.  相似文献   

Electron densities above a polar coronal hole based on improved Si  IX density diagnostics     

Doyle  J.G.  Keenan  F.P.  Ryans  R.S.I.  Aggarwal  K.M.  Fludra  A. 《Solar physics》1999,188(1):73-80

Using new close-coupling excitation rates for the C-like ion Siix, density-diagnostic ratios based on Siix lines have been re-evaluated and applied to a sequence of CDS observations taken above a polar coronal hole. The derived electron densities are in excellent agreement with previous values of N_eestimated from the N-like ion Siviii for another coronal hole. The confirmed trend is for a fall-off of one order of magnitude within the first 0.3 Rabove the limb. These densities are well fitted with an analytic formula for the density profile out to at least 8 R, by which stage the electron density has fallen to 4×10³ cm^–3, from 1.5×10⁸ cm^–3at 1.0 R.  相似文献   

Robe’s restricted problem of 2+2 bodies when the bigger primary is a Roche ellipsoid and the smaller primary is an oblate body     

Bhavneet Kaur  Rajiv Aggarwal 《Astrophysics and Space Science》2014,349(1):57-69

In this problem, one of the primaries of mass m ₁ is a Roche ellipsoid filled with a homogeneous incompressible fluid of density ρ ₁. The smaller primary of mass m ₂ is an oblate body outside the Ellipsoid. The third and the fourth bodies (of mass m ₃ and m ₄ respectively) are small solid spheres of density ρ ₃ and ρ ₄ respectively inside the Ellipsoid, with the assumption that the mass and the radius of the third and the fourth body are infinitesimal. We assume that m ₂ is describing a circle around m ₁. The masses m ₃ and m ₄ mutually attract each other, do not influence the motions of m ₁ and m ₂ but are influenced by them. We have extended the Robe’s restricted three-body problem to 2+2 body problem under the assumption that the fluid body assumes the shape of the Roche ellipsoid (Chandrashekhar in Ellipsoidal figures of equilibrium, Chap. 8, Dover, New York, 1987). We have taken into consideration all the three components of the pressure field in deriving the expression for the buoyancy force viz (i) due to the own gravitational field of the fluid (ii) that originating in the attraction of m ₂ (iii) that arising from the centrifugal force. In this paper, equilibrium solutions of m ₃ and m ₄ and their linear stability are analyzed. We have proved that there exist only six equilibrium solutions of the system, provided they lie within the Roche ellipsoid. In a system where the primaries are considered as Earth-Moon and m ₃,m ₄ as submarines, the equilibrium solutions of m ₃ and m ₄ respectively when the displacement is given in the direction of x ₁-axis or x ₂-axis are unstable.  相似文献