Bulge Size Research Articles

Galaxy Zoo: constraining the origin of spiral arms

Since the discovery that the majority of low-redshift galaxies exhibit some level of spiral structure, a number of theories have been proposed as to why these patterns exist. A popular explanation is a process known as swing amplification, yet there is no observational evidence to prove that such a mechanism is at play. By using a number of measured properties of galaxies, and scaling relations where there are no direct measurements, we model samples of SDSS and S$^4$G spiral galaxies in terms of their relative halo, bulge and disc mass and size. Using these models, we test predictions of swing amplification theory with respect to directly measured spiral arm numbers from Galaxy Zoo 2. We find that neither a universal cored or cuspy inner dark matter profile can correctly predict observed numbers of arms in galaxies. However, by invoking a halo contraction/expansion model, a clear bimodality in the spiral galaxy population emerges. Approximately 40 per cent of unbarred spiral galaxies at $z \lesssim 0.1$ and $\mathrm{M_*} \gtrsim 10^{10} \mathrm{M_\odot}$ have spiral arms that can be modelled by swing amplification. This population display a significant correlation between predicted and observed spiral arm numbers, evidence that they are swing amplified modes. The remainder are dominated by two-arm systems for which the model predicts significantly higher arm numbers. These are likely driven by tidal interactions or other mechanisms.

Quartz grainsize evolution during dynamic recrystallization across a natural shear zone boundary

Although it is widely accepted that grainsize reduction by dynamic recrystallization can lead to strain localization, the details of the grainsize evolution during dynamic recrystallization remain unclear. We investigated the bulge size and grainsizes of quartz at approximately the initiation and the completion stages of bulging recrystallization across the upper boundary of a 500 m thick mylonite zone above the Vincent fault in the San Gabriel Mountains, southern California. Within uncertainty, the average bulge size of quartz, 4.7 ± 1.5 μm, is the same as the recrystallized grainsize, 4.5 ± 1.5 μm, at the incipient stage of dynamic recrystallization, and also the same within uncertainties as the recrystallized grainsize when dynamic recrystallization is largely complete, 4.7 ± 1.3 μm. These observations indicate that the recrystallized grainsize is controlled by the nucleation process and does not change afterwards. It is also consistent with the experimental finding that the quartz recrystallized grainsize paleopiezometer is independent of temperature.

Stress dependence of microstructures in experimentally deformed calcite

Optical measurements of microstructural features in experimentally deformed Carrara marble help define their dependence on stress. These features include dynamically recrystallized grain size (Dr), subgrain size (Sg), minimum bulge size (Lρ), and the maximum scale length for surface-energy driven grain-boundary migration (Lγ). Taken together with previously published data Dr defines a paleopiezometer over the range 15–291 MPa and temperature over the range 500–1000 °C, with a stress exponent of −1.09 (CI −1.27 to −0.95), showing no detectable dependence on temperature. Sg and Dr measured in the same samples are closely similar in size, suggesting that the new grains did not grow significantly after nucleation. Lρ and Lγ measured on each sample define a relationship to stress with an exponent of approximately −1.6, which helps define the boundary between a region of dominant strain-energy-driven grain-boundary migration at high stress, from a region of dominant surface-energy-driven grain-boundary migration at low stress.

Zinc Ion-Dependent Peptide Nucleic Acid-Based Artificial Enzyme that Cleaves RNA-Bulge Size and Sequence Dependence.

In this report, we investigate the efficiency and selectivity of a Zn2+-dependent peptide nucleic acid-based artificial ribonuclease (PNAzyme) that cleaves RNA target sequences. The target RNAs are varied to form different sizes (3 and 4 nucleotides, nt) and sequences in the bulge formed upon binding to the PNAzyme. PNAzyme-promoted cleavage of the target RNAs was observed and variation of the substrate showed a clear dependence on the sequence and size of the bulge. For targets that form 4-nt bulges, we identified systems with an improved efficacy (an estimated half-life of ca 7–8 h as compared to 11–12 h for sequences studied earlier) as well as systems with an improved site selectivity (up to over 70% cleavage at a single site as compared to 50–60% with previous targets sequences). For targets forming 3-nt bulges, the enhancement compared to previous systems was even more pronounced. Compared to a starting point of targets forming 3-nt AAA bulges (half-lives of ca 21–24 h), we could identify target sequences that were cleaved with half-lives three times lower (ca 7–8 h), i.e., at rates similar to those found for the fastest 4-nt bulge system. In addition, with the 3-nt bulge RNA target site selectivity was improved even further to reach well over 80% cleavage at a specific site.

Treatment of lumbar degenerative disc disease-associated radicular pain with culture-expanded autologous mesenchymal stem cells: a pilot study on safety and efficacy

BackgroundDegenerative disc disease (DDD) is a common cause of lower back pain with radicular symptoms and has a significant socioeconomic impact given the associated disability. Limited effective conservative therapeutic options result in many turning to surgical alternatives for management, which vary in the rate of success and also carry an increased risk of morbidity and mortality associated with the procedures. Several animal based studies and a few human pilot studies have demonstrated safety and suggest efficacy in the treatment of DDD with mesenchymal stem cells (MSCs). The use of bone marrow-derived MSCs for the treatment of DDD is promising and in the present study we report on the safety and efficacy findings from a registry based proof of concept study using a percutaneous intradiscal injection of cultured MSCs for the management of DDD with associated radicular symptoms.MethodsThirty-three patients with lower back pain and disc degeneration with a posterior disc bulge diagnosed on magnetic resonance imaging (MRI) met the inclusion criteria and were treated with culture-expanded, autologous, bone marrow-derived MSCs. Prospective registry data was obtained at multiple time intervals up to 6 years post-treatment. Collected outcomes included numeric pain score (NPS), a modified single assessment numeric evaluation (SANE) rating, functional rating index (FRI), measurement of the intervertebral disc posterior dimension, and adverse events.ResultsThree patients reported pain related to procedure that resolved. There were no serious adverse events (i.e. death, infection, or tumor) associated with the procedure. NPS change scores relative to baseline were significant at 3, 36, 48, 60, and 72 months post-treatment. The average modified SANE ratings showed a mean improvement of 60% at 3 years post-treatment. FRI post-treatment change score averages exceeded the minimal clinically important difference at all time points except 12 months. Twenty of the patients treated underwent post-treatment MRI and 85% had a reduction in disc bulge size, with an average reduction size of 23% post-treatment.ConclusionsPatients treated with autologous cultured MSCs for lower back pain with radicular symptoms in the setting of DDD reported minor adverse events and significant improvements in pain, function, and overall subjective improvement through 6 years of follow-up.NCT03011398. A Clinical Registry of Orthobiologics Procedures. https://clinicaltrials.gov/ct2/show/NCT03011398?term=orthobiologics&rank=1

THE DEMOGRAPHICS OF GALACTIC BULGES IN THE SDSS DATABASE

ABSTRACT We present a new database of our two-dimensional bulge–disk decompositions for 14,233 galaxies drawn from Sloan Digital Sky Survey DR12 in order to examine the properties of bulges residing in the local universe (0.005 < z < 0.05). We performed decompositions in the g and r bands by utilizing the galfit software. The bulge colors and bulge-to-total ratios are found to be sensitive to the details in the decomposition technique, and hence we hereby provide full details of our method. The g − r colors of bulges derived are almost constantly red regardless of bulge size, except for the bulges in the low bulge-to-total ratio galaxies (B/T r ≲ 0.3). Bulges exhibit similar scaling relations to those followed by elliptical galaxies, but the bulges in galaxies with lower bulge-to-total ratios clearly show a gradually larger departure in slope from the elliptical galaxy sequence. The scatters around the scaling relations are also larger for the bulges in galaxies with lower bulge-to-total ratios. Both the departure in slopes and larger scatters likely originate from the presence of young stars. The bulges in galaxies with low bulge-to-total ratios show signs of a frosting of young stars so substantial that their luminosity-weighted Balmer-line ages are as small as 1 Gyr in some cases. While bulges seem largely similar in optical properties to elliptical galaxies, they do show clear and systematic departures as a function of bulge-to-total ratio. The stellar properties and perhaps associated formation processes of bulges seem much more diverse than those of elliptical galaxies.

Spin-up of massive classical bulges during secular evolution

Classical bulges in spiral galaxies are known to rotate but the origin of this observed rotational motion is not well understood. It has been shown recently that a low-mass classical bulge (ClB) in a barred galaxy can acquire rotation from absorbing a significant fraction of the angular momentum emitted by the bar. Our aim here is to investigate whether bars can spin up also more massive ClBs during the secular evolution of the bar, and to study the kinematics and dynamics of these ClBs. We use a set of self-consistent N-body simulations to study the interaction of ClBs with a bar that forms self-consistently in the disk. We use orbital spectral analysis to investigate the angular momentum gain by the classical bulge stars. We show that the ClBs gain, on average, about 2 - 6% of the disk's initial angular momentum within the bar region. Most of this angular momentum gain occurs via low-order resonances, particularly 5:2 resonant orbits. A density wake forms in the ClB which corotates and aligns with the bar at the end of the evolution. The spin-up process creates a characteristic linear rotation profile and mild tangential anisotropy in the ClB. The induced rotation is small in the centre but significant beyond $\sim2$ bulge half mass radii, where it leads to mass-weighted $V/\sigma \sim 0.2$, and reaches a local $V_{max}/\sigma_{in} \sim 0.5$ at around the scale of the bar. The resulting $V/\sigma$ is tightly correlated with the ratio of the bulge size to the bar size. In all models, a box/peanut bulge forms suggesting that composite bulges may be common. Bar-bulge resonant interaction in barred galaxies can provide some spin up of massive ClBs, but the process appears to be less efficient than for low-mass ClBs. Further angular momentum transfer due to nuclear bars or gas inflow would be required to explain the observed rotation if it is not primordial.

3D numerical simulation and analysis of railgun gouging mechanism

Abstract A gouging phenomenon with a hypervelocity sliding electrical contact in railgun not only shortens the rail lifetime but also affects the interior ballistic performance. In this paper, a 3-D numerical model was introduced to simulate and analyze the generation mechanism and evolution of the rail gouging phenomenon. The results show that a rail surface bulge is an important factor to induce gouging. High density and high pressure material flow on the contact surface, obliquely extruded into the rail when accelerating the armature to a high velocity, can produce gouging. Both controlling the bulge size to a certain range and selecting suitable materials for rail surface coating will suppress the formation of gouging. The numerical simulation had a good agreement with experiments, which validated the computing model and methodology are reliable.

Thermodynamic examination of 1- to 5-nt purine bulge loops in RNA and DNA constructs.

Bulge loops are common features of RNA structures that are involved in the formation of RNA tertiary structures and are often sites for interactions with proteins and ions. Minimal thermodynamic data currently exist on the bulge size and sequence effects. Using thermal denaturation methods, thermodynamic properties of 1- to 5-nt adenine and guanine bulge loop constructs were examined in 10 mM MgCl2 or 1 M KCl. The loop parameters for 1- to 5-nt purine bulge loops in RNA constructs were between 3.07 and 5.31 kcal/mol in 1 M KCl buffer. In 10 mM magnesium ions, the ΔΔG° values relative to 1 M KCl were 0.47–2.06 kcal/mol more favorable for the RNA bulge loops. The loop parameters for 1- to 5-nt purine bulge loops in DNA constructs were between 4.54 and 5.89 kcal/mol. Only 4- and 5-nt guanine constructs showed significant change in stability for the DNA constructs in magnesium ions. A linear correlation is seen between the size of the bulge loop and its stability. New prediction models are proposed for 1- to 5-nt purine bulge loops in RNA and DNA in 1 M KCl. We show that a significant stabilization is seen for small bulge loops in RNA in the presence of magnesium ions. A prediction model is also proposed for 1- to 5-nt purine bulge loop RNA constructs in 10 mM magnesium chloride.

Cis regulatory effects on A-to-I RNA editing in related Drosophila species.

Adenosine-to-inosine RNA editing modifies maturing mRNAs through the binding of adenosine deaminase acting on RNA (Adar) proteins to double-stranded RNA structures in a process critical for neuronal function. Editing levels at individual editing sites span a broad range and are mediated by both cis-acting elements (surrounding RNA sequence and secondary structure) and trans-acting factors. Here, we aim to determine the roles that cis-acting elements and trans-acting factors play in regulating editing levels. Using two closely related Drosophila species, D. melanogaster and D. sechellia, and their F1 hybrids, we dissect the effects of cis sequences from trans regulators on editing levels by comparing species-specific editing in parents and their hybrids. We report that cis sequence differences are largely responsible for editing level differences between these two Drosophila species. This study presents evidence for cis sequence and structure changes as the dominant evolutionary force that modulates RNA editing levels between these Drosophila species.

AGN spiral galaxies in groups: effects of bars

We explore properties of barred active spiral galaxies in groups selected from the SDSS-DR7, with the aim of assessing the effects of bars on AGN and the role of the high density environment. We identified barred active galaxies that reside in groups from SDSS-DR7 group catalog. To provide a suitable quantification of the effects of bars, a reliable control sample of unbarred active galaxies in high density environments with similar redshift, magnitude, morphology, and bulge size distributions was constructed. We found that the fraction of barred AGN galaxies in groups (~ 38 %) is higher than those in the total barred AGN sample ( ~ 28 %), indicating that AGN spiral galaxies in groups are more likely to be barred than those in the field. We also found that barred AGN galaxies are more concentrated towards the group centers than the other unbarred AGN group members. In addition, barred AGN host galaxies show an excess of population dominated by red colors suggesting that bars produce an importanteffect on galaxy colors of AGN hosts. The host groups of the barred AGN exhibit a larger fraction of red colors than the host groups of the corresponding unbarred active galaxies. Color-magnitude relations of both host groups of AGN differ significantly: the host group colors of barred active galaxies display distributions spreading toward red populations, with respect to the host groups of the unbarred AGN objects. Barred active galaxies show an excess of nuclear activity compared to galaxies without bars. We found that barred active galaxies located farther from the group-center have stronger Lum[OIII]. Our findings suggest that the efficiency of bars to transport material towards the more central regions of the AGN galaxies in high density environments reveals an important dependence on the localization of objects within the group and on the host group colors.

The binding energies of a bulged GaAs nanowire

As it is well-known the electronic structure of the semiconductor nanostructures are so sensitive to alteration of confinement while the nanostructure morphology often determines the confinement. Accordingly existence of a bulge on the wire surface will affect the features of the nanowire. In the present work we consider an on-center hydrogenic donor impurity in a GaAs nanowire with bulge. The ground and first excited states energy levels as well as their binding energies are calculated as functions of bulge and nanowire radius. It is found that both the energy levels and binding energies are strongly influenced by the bulge size for ultrafine nanowires. For large wire radii the effects of bulge existence is trivial and the electronic properties of the system approach to those of the simple nanowire.

The decomposed bulge and disc size–mass relations of massive galaxies at 1 < z < 3 in CANDELS

We have constructed a mass-selected sample of Mstar>10^11Msolar galaxies at 1<z<3 in the CANDELS UDS and COSMOS fields and have decomposed these systems into their separate bulge and disk components according to their H(160)-band morphologies. By extending this analysis to multiple bands we have been able to conduct individual bulge and disk component SED fitting which has provided us with stellar-mass and star-formation rate estimates for the separate bulge and disk components. These have been combined with size measurements to explore the evolution of these massive high-redshift galaxies. By utilising the new decomposed stellar-mass estimates, we confirm that the bulge components display a stronger size evolution than the disks. This can be seen from both the fraction of bulge components which lie below the local relation and the median sizes of the bulge components, where the bulges are a median factor of 2.93+/-0.32 times smaller than similarly massive local galaxies at 1<z<2 and 3.41+/-0.58 smaller at 2<z<3; for the disks the corresponding factors are 1.65+/-0.14 and 1.99+/-0.25. Moreover, by splitting our sample into the passive and star-forming bulge and disk sub-populations and examining their sizes as a fraction of their present-day counter-parts, we find that the star-forming and passive bulges are equally compact, star-forming disks are larger, while the passive disks have intermediate sizes. This trend is not evident when classifying galaxy morphology on the basis of single-Sersic fits and adopting the overall star-formation rates. Finally, by evolving the star-formation histories of the passive disks back to the redshifts when the passive disks were last active, we show that the passive and star-forming disks have consistent sizes at the relevant epoch. These trends need to be reproduced by any mechanisms which attempt to explain the morphological evolution of galaxies.

X-RAY NUCLEAR ACTIVITY IN S4G BARRED GALAXIES: NO LINK BETWEEN BAR STRENGTH AND CO-OCCURRENT SUPERMASSIVE BLACK HOLE FUELING

Stellar bars can lead to gas inflow toward the center of a galaxy and stimulate nuclear star formation. However, there is no compelling evidence on whether they also feed a central supermassive black hole: by measuring the fractions of barred active and inactive galaxies, previous studies have yielded conflicting results. In this paper, we aim to understand the lack of observational evidence for bar-driven active galactic nucleus (AGN) activity by studying a sample of 41 nearby (d < 35 Mpc) barred galaxies from the Spitzer Survey for Stellar Structure in Galaxies. We use Chandra observations to measure nuclear 2--10 keV X-ray luminosities and estimate Eddington ratios, together with Spitzer 3.6um imaging to quantify the strength of the stellar bar in two independent ways: (1) from its structure, as traced by its ellipticity and boxiness, and (2) from its gravitational torque Q_b, taken as the maximum ratio of the tangential force to the mean background radial force. In this way, rather than discretizing the presence of both stellar bars and nuclear activity, we are able to account for the continuum of bar strengths and degrees of AGN activity. We find nuclear X-ray sources in 31 out of 41 galaxies with median X-ray luminosity and Eddington ratio of L_X=4.3x10^{38} erg/s and L_bol/L_Edd=6.9x10^{-6} respectively, consistent with low-luminosity AGN activity. Including upper limits for those galaxies without nuclear detections, we find no significant correlation between any of the bar strength indicators and the degree of nuclear activity, irrespective of galaxy luminosity, stellar mass, Hubble type, or bulge size. Strong bars do not favor brighter or more efficient nuclear activity, implying that at least for the low-luminosity regime, supermassive black hole fueling is not closely connected to large scale features.

Characteristics of right ventricular free wall motion in young patients with ventricular arrhythmia, a cardiac MRI study

Background Right ventricular (RV) regional wall characteristics are important in CMR evaluation for arrhythmogenic RV dysplasia (ARVD). While some features are well defined, others are of uncertain clinical significance, due in part, to the high prevalence of RV wall motion variants found in normal subjects. In this study we performed a retrospective review of RV free wall characteristics in a large cohort of young patients referred for ventricular arrhythmia evaluation and compared the findings with an age-matched normal cohort. Methods The study consisted of 159 consecutive patients aged 18 to 49 years referred for CMR due to ventricular arrhythmias and 51 age-matched normal controls. All subjects underwent CMR. Cine images of the 4-chamber view were reviewed to characterize the RV wall motion as having bulge or outpouching at end systole or at end diastole. The bulges were further classified by location, size and relationship to the moderator band. The size of bulges were graded as small (≤0.5 cm 2 ), moderate (0.5 1c m 2 ) and large (> 1 cm 2 ). Results Mean age was 38 years. Of the 159 patients, 62 (39%) presented with premature ventricular contractions (PVCs) and 97 (61%) with ventricular tachycardia (VT). There was no significant difference in RV size and function between patients and controls. Diastolic bulges were most common in the VT group (10 cases, 10%), rare in PVC and control group (1 case each, 2%). Large diastolic bulges were present only in 6 VT group cases. Systolic bulges were more common, with 11/51 (22%) in normal control, 5/62 (8%) in PVC group and 20/97 (21%) in VT group. All systolic bulges in the control group were small while bulge size was mainly moderate in the PVC group (4/5) and large bulges were only present in the VT group (4/20). All systolic bulges were in close proximity to a moderator band in the control group but 6/34 (18%) were not in the arrhythmic groups. Basal location is uncommon but 5 of 6 cases were found in the VT group, 1 in the PVC group and none in the control group. Conclusions RV characteristics that are predominantly associated with VT include bulges or outpouchings present in diastole, basal location, large size and in the absence of a relation to the moderator band. Our findings suggest that risk stratification of ventricular arrhythmia should consider those RV features particularly in cases where the diagnostic criteria of ARVD are unmet. Funding None.

Crystal Growth during the Solidification Process of Continuous Casting Slab

Under the condition that the solid-liquid interface bends periodically in continuous casting, the expression of solid-phase growth rate adapting to continuous casting was set up, and then the growth rates were calculated. On this basis, the morphologic of crystal growth and the variation of primary dendrite spacing during continuous casting slabs were studied. The results show that the growth rate is the fastest when solid-phase moves to wave crest within a deformation periodicity, whereas the growth rate is the slowest when the crystal moves to wave hollow. The bigger the bulge size is, the greater the variation amplitude of the growth rate will become. The variation of the growth rate results in the S/L interface to develop towards a planar surface. Because the value is much smaller than the critical value of the transformation from cells to dendrites, and the crystals only grow in the fashion of dendrites. The primary dendrite spacing at wave crest is bigger than the primary dendrite spacing at wave hollow in early stage of columnar crystal growth, and the dendrite spacing at wave crest is basically equal with the dendrite spacing at wave hollow in the late stage of solidification, and they quickly simultaneous increase. Good correlation is obtained between the experimental results and the calculation results of the dendrite arm spacing.

Time-dependent Benioff strain release diagrams

New time-dependent Benioff strain (TDBS) release diagrams were analyzed for acoustic emission during various loading tests and for electromagnetic (EM) radiation emanating during compression and, tension, which end in failure. TDBS diagrams are Benioff diagrams that are built consecutively, each time using a greater number of events (acoustic or EM emissions) using the last event as if it were associated with the ‘actual failure’. An examination of such TDBS diagrams shows that at a certain time point (this time point is denoted by the term ‘alarm’ time), a comparatively short interval prior to actual collapse, their decreasing part is broken by a positive ‘bulge’. This ‘bulge’ is quantified and an algorithm proposed for its assessment. Using the alarm time and other parameters of the failure process (fall, bulge size and escalation factors, bulge slope and slope fall time), a criterion for estimating the time of the actual collapse is developed and shown to agree well with laboratory experimental results.

RNA helical imperfections regulate activation of the protein kinase PKR: Effects of bulge position, size, and geometry

The protein kinase, PKR, is activated by long stretches of double-stranded (ds) RNA. Viruses often make long dsRNA elements with imperfections that still activate PKR. However, due to the complexity of the RNA structure, prediction of whether a given RNA is an activator of PKR is difficult. Herein, we systematically investigated how various RNA secondary structure defects contained within model dsRNA affect PKR activation. We find that bulges increasingly disfavor activation as they are moved toward the center of a duplex and as they are increased in size. Model RNAs designed to conform to cis, trans, or bent global geometries through strategic positioning of one or more bulges decreased activation of PKR relative to perfect dsRNA, although cis-bulged RNAs activated PKR much more potently than trans-bulged RNAs. Activation studies on bulge-containing chimeric duplexes support a model wherein PKR monomers interact adjacently, rather than through-space, for activation on bulged substrates. Last, unusually low ionic strength induced substantial increases in PKR activation in the presence of bulged RNAs suggesting that discrimination against bulges is higher under biological ionic strength conditions. Overall, this study provides a set of rules for understanding how secondary structural defects affect PKR activity.

Dynamics of binary compact massive objects in galactic nuclei during interactions with globular clusters

The migration of binary systems of compact massive objects in galactic nuclei owing to encounters with globular clusters is studied. A binary moves in the field of a galactic bulge with a fixed potential. An empirical relationship between the masses of the binary and bulge of the form M b = 1000(M 1+M 2) is used, where M 1 and M 2 are the masses of the components of the binary. The amplitude of the drift of the binary components is found as a function of the initial binary orbit parameters, the size of the bulge, and the initial velocity and mass of the globular cluster. It is shown that the amplitude of the drift depends to a greater extent on the parameters of the cluster, while the magnitude of the perturbation in the binary orbit depends weakly on the bulge size and the eccentricity and major semiaxis of the binary orbit. The amplitude of the drift of the center of mass also decreases on the average as the difference between the masses of the components becomes larger.

Thermodynamic stablity and divalent ion interactions of RNA containing purine‐rich bulges

Bulges are a common non‐helical motif found in RNA that play an important role in RNA recognition. Small asymmetrical bulges occur in many different RNA including HIV‐RNA and various microRNA. In HIV‐1 TAR RNA, a trinucleotide bulge interacts with the Tat protein of HIV‐1 to increase its rate of transcription one hundred fold. Previous studies in our lab have shown that TAR RNA containing cytosine‐rich trinucleotide bulges are ~2 kcal/mol more stable than those containing uracil‐rich bulges, in 1 M KCl conditions. Magnesium ions stabilize TAR RNA containing uracil‐rich bulges by ~1–2 kcal/mol and cytosine‐rich bulges by ~ 1 kcal/mol, relative to 1 M KCl conditions. In this study, we are examining the differences in RNA stability as the bulge size is varied between one and five nucleotides. Thermal denaturation experiments are being performed on varying concentrations of RNA in buffers containing 1 M KCl or varying concentrations of divalent ions. Altering the nucleotide sequence of the bulge alters RNA stability as well as its ion binding properties. A comparison of thermodynamic properties of purine‐ and pyrimidine‐rich bulges will be presented. This work was funded by NSF MCB‐0621509 to NG.