New Jersey Institute of Technology (NJIT) is a public research university in Newark, New Jersey. NJIT offers 100 degree programs in 27 undergraduate majors and 30 graduate specialties.
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The Neighborhood Auditing Tool James Geller
Michael Halper
Yehoshua Perl
C. Paul Morrey
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Lubricated Transport DD Joseph, May 2000 Office of Basic Energy Sciences, Engineering, DOE
Lubricated Transport DD Joseph, May 2000 Office of Basic Energy Sciences, Engineering, DOE
Some flow types
Ideal core-annual flow
Laminar and turbulent core flow
Wavy core flow
Instability of smooth waves
Waves shortening and sharkskin
Movie of wave shortening
Self lubrication (w/o emulsions)
Self-lubrication of bitumen froth
Self-lubrication of midway sunset crude
Lubrication of concentrated o/w emulsions
Rheometer studies
Comparison of rheometer and pipeline data
Lubrication of solids in liquids
Steep waves
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Coxsackie Virus and its effect on the Arf1 protein Ani Chintalapani & Matthew Hanna A joyous day in the Life Science Center of Rutgers Newark
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V.I. Abramenko, V.B. Yurchyshyn, H. Wang , T.R. Spirock, P.R. Goode
Big Bear Solar Observatory, NJIT
Crimean Astrophysical Observatory, Ukraine
Email: avi@bbso.njit.edu
V.I. Abramenko, V.B. Yurchyshyn, H. Wang , T.R. Spirock, P.R. Goode
Big Bear Solar Observatory, NJIT
Crimean Astrophysical Observatory, Ukraine
Email: avi@bbso.njit.edu
34th Meeting of SPD
16-29 June 2003
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Signature of Avalanche in Solar Flares as Measured by Photospheric Magnetic Fields V.I. Abramenko, V.B. Yurchyshyn, H. Wang , T.R. Spirock, P.R. Goode
Big Bear Solar Observatory, NJIT
Crimean Astrophysical Observatory, Ukraine
Email: avi@bbso.njit.edu
Signature of Avalanche in Solar Flares as Measured by Photospheric Magnetic Fields V.I. Abramenko, V.B. Yurchyshyn, H. Wang , T.R. Spirock, P.R. Goode
Big Bear Solar Observatory, NJIT
Crimean Astrophysical Observatory, Ukraine
Email: avi@bbso.njit.edu
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Magnetic Structures of Active Regions and their Link to Coronal Mass Ejections Vasyl Yurchyshyn, Big Bear Solar Observatory, Big Bear City, CA 92314, www.bbso.njit.edu/~vayur Bz 55 deg
(MFI) MC axis The active region’s magnetic field was mainly NS orientated and the left handed twist caused its axial field to be directed eastwardly. Because the ejecta had southwardly directed azimuthal component, this eruption was associated with a very strong geomagnetic storm. CME on July 14, 2000 – Bastille Day Flare CME on February 17, 2000 Bz 85 deg
(MFI) MC axis The erupted filament D had the SN orientation, i.e. its axial field was directed northward. This AR was positively twisted and the azimuthal field was directed westward. This eruption did not cause any geomagnetic activity because no strong southwardly directed magnetic component was present in the erupted field. October 28 2003 X17 Event November 18, 2003 M5.7 Flare and CME Solar coronal mass ejections (CMEs) are a principal link that connect the chain of events in the solar atmosphere, interplanetary space and the earth's magnetosphere. When CMEs reach the earth, they may cause a significant magnetic perturbations, provided that their magnetic environment contains intensive southward magnetic fields. Earlier studies unanimously suggest that there is a correspondence between the erupted filaments and magnetic clouds (MC) at 1AU. Our study shows that in the case of active regions the...
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F2 Photospheric Sources of Very Fast (>1000km/s) Coronal Mass Ejections We identified photospheric sources of 39 very fast CMEs and we distinguished three different groups of active regions with specific magnetic configurations:
i) complex delta spots; ii) simple tadpole-shaped delta spots and iii) magnetic complexes. Vasyl Yurchyshyn, Big Bear Solar Observatory, 40386 North Shore Lane, Big Bear City, CA 92314 email: vayur@bbso.njit.edu, http://www.bbso.njit.edu/~vayur 1. CME projection speed seem to be related to the Bz in IMF : The hourly averaged Bz at the front of an ejecta (ACE, GSM) vs the projected speed of CMEs. Solid line is an exponential fit (F1): Bz[nT]=12.3+0.7exp(V/404). (r.m.s=7nT) The Dst index plotted vs the hourly averaged Bz. The solid line is a 3rd degree polinominal fit, F2, and the dashed lines show r.m.s=33nT. 2. In turn, the Bz in IMF defines the intensity (the Dst Index) of a storm F1 SHINE It seems that only fast CMEs capable of producing strong geomagnetic storms. If so, where these fast CMEs originate? 1. Complex Delta Spots (11 - X, 8 - M & 2 – C flare) Date Speed Coord NOAA Area Length Flare The M7.9 Flare in NOAA AR 9415 on April 9th, 2001 Pre-flare Configuration Post-flare Configuration CME PFL MC at 1AU CME near the Sun Is magnetic complexity crucial for production of a fast CME? Yes
Is reconnection required to produce a fast CME? Yes 2. Tadpole-Shaped ARs (2 - X, 5 - M &...
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How the Intensity of Geomagnetic Storms can be Determined from Solar Data Coronal Mass Ejections (CMEs) are correlated with geomagnetic storms, which are a response of the magnetosphere to an action of the southward interplanetary magnetic field (IMF). We discuss a new method to produce forecast of the intensity of a geomagnetic storm at least 1 day in advance based solar data. Vasyl Yurchyshyn, Big Bear Solar Observatory, 40386 North Shore Lane, Big Bear City, CA 92314, vayur@bbso.njit.edu 1. We found that the CME projection speed is related to the Bz in IMF : Fig. 1 The hourly averaged Bz measured at the front of an ejecta (ACE, GSM) vs the projected speed of CMEs. The solid line is an exponential fit: F1=Bz[nT]=12.3+0.7exp(V/404). The dashed lines show r.m.s=7nT. 2. In turn, the Bz in IMF defines the intensity (the Dst Index) of a storm Fig. 2 The Dst index vs the hourly averaged Bz. The solid line is a 3rd degree polinominal fit, F2, and the dashed lines show r.m.s=33nT. The X4.5/3B flare at 18:46UT on March 10, 1989 produced 1st CME, which arrived on March 13 at 02:00UT. Its travel speed was about 760km/s, while the initial speed was 1000km/s.
Bz predicted: -10 … -24 nT
Dst predicted: -100 … -180 nT The X1.0/2B flare on March 11 at 15:33UT produced 2nd CME, which arrived on March 13 at 10:00UT. Its travel speed was about 990km/s, while the initial speed was 1100km/s.
Bz predicted: -13 … -27 nT
Dst predicted: (-120 … -190)+ΔDst1 = -210…-280 ΔDs...
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Statistical Distributions of Speeds of Coronal Mass Ejections 1Big Bear Solar Obs, Big Bear , CA 92314; 2Catholic University of America, Washington DC 20064; 3New Jersey Inst. of Technology, Newark, NJ 07102; 4NASA/GSFC, Greenbelt, MD 20771 Vasyl Yurchyshyn1, Seiji Yashiro2, Valentyna Abramenko1, Haimin Wang3, Nat Gopalswamy4 Decelerating
CMEs Accelerating
CMEs We analyzed the distribution of speeds of 4315 CMEs published in The CME Catalog at the CDAW data center. We found that the speed distributions for accelerating and decelerating events are nearly identical (2=0.0033) and to a good approximation they can be fitted with a single log-normal distribution. This finding implies that, statistically, there is no physical distinction between the accelerating and the decelerating events.The log-normal distribution of CME speeds suggests that the same driving mechanism of a non-linear nature is acting in both slow and fast dynamical types of CMEs. liner-liner representation of the distribution of the number of CMEs, N, versus their speeds, v, determined from the linear fit log-liner representation of the above distribution can
be modeled by a
normal (gaussian) approximation The skewed form of the distribution suggests that it may be modeled either with a single log-normal distribution or a sum of a log-normal and a Gaussian distributions. It is said that if a random variable (in our case the speed of a CME) is log-normally distributed then its natural logarithm...
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Rapid Changes in the Longitudinal Magnetic Field Associated with the July 23 2002 gamma-ray Flare Vasyl Yurchyshyn, Haimin Wang, Valentyna Abramenko,
Thomas J. Spirock and Säm Krucker
Big Bear Solar Observatory, Big Bear City, CA 92314
Space Sciences Lab, University of California, Berkeley, CA 94720
Rapid Changes in the Longitudinal Magnetic Field Associated with the July 23 2002 gamma-ray Flare Vasyl Yurchyshyn, Haimin Wang, Valentyna Abramenko,
Thomas J. Spirock and Säm Krucker
Big Bear Solar Observatory, Big Bear City, CA 92314
Space Sciences Lab, University of California, Berkeley, CA 94720
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Coronal Ejecta in October - November of 2003 and predictions of the associated geomagnetic events 1Big Bear Solar Observatory, New Jersey Institute of Technology, http://www.bbso.njit.edu/~vayur 2Institute of Geophysics and Planetary Physics, University of California, Riverside, http://www.igpp.ucr.edu We have found recently that the intensity of Bz in the IMF is correlated with the plane of sky speed of coronal mass ejections (CMEs)1,2 . In turn, the Bz in the IMF is correlated with the Dst index of geomagnetic activity2,3,4,5.
Here we present results of prediction of the magnitude and the orientation of the Bz and the Dst index made for 3 halo CMEs erupted on October 28 (event I), October 29 (event II) and November 18 (event III) of 2003. The comparison between the predicted values and the observed data shows that we were able to successfully predict the magnitude of 2 out of 3 geomagnetic events (events I and II), while we have underestimated the magnitude of the Dst index for the event III on November 18 2003. Vasyl Yurchyshyn Qiang Hu Event I:
The X17.2/4B flare started at 0951UT on Oct 28 2003 and it was associated with a halo CME. The clock angle (measured clockwise from the east) of the post flare loops system, associated with this CME, was about 215 deg and the erupted field had negative helicity . This suggests that the axial field of the CME may have a southward Bz component. The plane of sky speed of the CME was about 1500km/s. Based on this speed w...
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