Lena Murchikova's Home Page Lena (Elena M.) Murchikova's Home Page

I am a William D. Loughlin Member at the Institute for Advanced Study in Princeton, NJ

office: Bloomberg Hall 249
email: lena AT ias DOT edu

Mailing address
School of Natural Sciences
Institute for Advanced Study
Princeton, NJ 08540

Education
PhD, Astrophysics, California Institute of Technology
PhD, Particle Physics, Moscow State University
Specialist, Theoretical Physics, Moscow State University

Research Interests
I am a physicist working on a broad range of topics in astrophysics. My interests are primarily in black hole physics, Galactic Center black hole Sagittarius A* and its accretion, but also extend to exoplanets, star formation, and neutron stars.

My approach to astrophysics is problem oriented rather than tool oriented. This means that I apply, acquire and, if needed, develop the tools necessary to solve problems I work on. In my day to day research I use observations, simulation, and pen and paper theory. My Sagittarius A* projects heavily involve innovative algorithm development for processing of interferometric data which I apply mostly to the data from Atacama Large Millimeter/submillimeter Array (ALMA). As a Principal Investigator, I have been granted about 100 hours of ALMA time, which is worth approximately 2.5 million dollars.

In my past I used to write papers in elementary particle physics and string theory.

Other Interests
Private pilot. Avid mountaneer. Consulted on set of movie "Interstellar". Occasional (drone) photographer. Classical pianist.

IAS Astro learning seminar
Gravitational Waves
Plasma Physics

Some Recent Works
Full list of publications is available on ArXiv and ADS
(published as Lena Murchikova, Elena Murchikova and E.M. Murchikova)

Second Scale Submillimeter Variability of Sagittarius A* during flaring activity of 2019: On the Origin of Bright Near Infrared Flares
Lena Murchikova and Gunther Witzel, The Astrophysical Journal Letters (accepted)

In 2019, Sgr A* -- the supermassive black hole in the Galactic Center -- underwent unprecedented flaring activity, brightening by up to a factor of 100 compared to quiescent values. Here we report ALMA observations of Sgr A*'s continuum variability at 1.3 mm (230 GHz) -- a tracer of the accretion rate -- conducted one month after the brightest detected near infrared (NIR) and in the middle of the flaring activity of 2019. We develop an innovative light curve extraction technique which (together with ALMA's excellent sensitivity) allows us to obtain the light curves which are simultaneously of high time resolution (2 seconds) and high signal-to-noise ratio (~ 500). We construct an accurate intrinsic structure function of the Sgr A* submm variability, improving on previous studies by about two orders of magnitude in timescale and one order of magnitude in sensitivity. We compare the June 2019 variability behavior with that of 2001-2017, and suggest that the most likely cause of the bright NIR flares is magnetic reconnection.

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S0-2 star, G1- and G2-objects and flaring activity of the Milky Way's Galactic Center black hole in 2019
Lena Murchikova, The Astrophysical Journal Letters 910 L1 (2021)

In 2019, the Galactic center black hole Sgr A* produced an unusually high number of bright near-infrared flares, including the brightest-ever detected flare (Do et al 2019, Gravity 2020). We propose that this activity was triggered by the near simultaneous infall of material shed by G1 and G2 objects due to their interaction with the background accretion flow. We discuss mechanisms by which S-stars and G-objects shed material, and estimate both the quantity of material and the infall time to reach the black hole.

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Reconstructing EUV spectrum of star forming regions from millimeter recombination lines of HI, HeI, and HeII
Lena Murchikova, Eric J. Murphy, Dariusz C. Lis, Lee Armus, Nadia Zakamska et al, The Astrophysical Journal (2020)

The extreme ultraviolet (EUV) spectra of distant star-forming regions cannot be probed directly using either ground- or space-based telescopes due to the high cross-section for interaction of EUV photons with the interstellar medium. This makes EUV spectra poorly constrained. The mm/submm recombination lines of H and He, which can be observed from the ground, can serve as a reliable probe of the EUV. Here we present a study based on ALMA observations of three Galactic ultra-compact HII regions and the starburst region Sgr B2(M), in which we reconstruct the key parameters of the EUV spectra using mm recombination lines of HI, HeI and HeII. We find that in all cases the EUV spectra between 13.6 and 54.4 eV have similar frequency dependence: L_\nu ~ \nu^{-\gamma} ~\nu^{-4.5 +/- 0.4}. We compare the inferred values of the EUV spectral slopes with the values expected for a purely single stellar evolution model (Starburst99) and the Binary Population and Spectral Synthesis code (BPASS). We find that the observed spectral slope differs from the model predictions. This may imply that the fraction of interacting binaries in HII regions is substantially lower than assumed in BPASS. The technique demonstrated here allows one to deduce the EUV spectra of star forming regions providing critical insight into photon production rates at < 912 Angstrom and can serve as calibration to starburst synthesis models, improving our understanding of star formation in distant universe and the properties of ionizing flux during reionization.

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Peas in a Pod? Radius correlations in Kepler multi-planet systems
Lena Murchikova & Scott Tremaine, The Astronomical Journal (2020)

In this work we address the claim of Weiss et al. (2018) that the radii of adjacent planets in Kepler multi-planet systems are correlated. We explore two simple toy models---in the first the radii of the planets are chosen at random from a single universal distribution, and in the second we postulate several types of system with distinct radius distributions. We show that an apparent correlation between the radii of adjacent planets similar to the one reported by Weiss et al. (2018) can arise in both models. In addition the second model fits the radius and signal-to-noise distribution of the observed planets.

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A Cool Accretion Disk around the Galactic Centre Black Hole
Elena M. Murchikova, Anna Pancoast, E. Sterl Phinney, Roger D. Blandford, Nature (2019)

A supermassive black hole SgrA* with the mass ~4x10^6 Msun resides at the centre of our galaxy. Building up such a massive black hole within the ~10^10 year lifetime of our galaxy would require a mean accretion rate of ~4x10^-4 Msun/yr. At present, X-ray observations constrain the rate of hot gas accretion at the Bondi radius (10^5 R_Sch = 0.04 pc at 8kpc) to \dot{M}_Bondi ~ 3x10^-6 Msun/yr, and polarization measurements constrain it near the event horizon to \dot{M}_horizon ~ 10^{-8} Msun/yr. A range of models was developed to describe the accretion gas onto an underfed black hole. However, the exact physics still remains to be understood. One challenge with the radiation inefficient accretion flows is that even if one understands the dynamics there is no accepted prescription for associating emissivity (and absorption) with the flow. The other issue is the lack of model-independent probes of accretion flow at intermediate radii (between few and ~ 10^5 R_Sch), i.e. the constraints that do not assume a model of accretion flow as an input parameter. We report detection and imaging of the 10^4 K ionized gas disk within 2x10^4 R_Sch in a mm hydrogen recombination line H30alpha: n = 31 -> 30 at 231.9 GHz using the ALMA. The emission was detected with a double-peaked line profile spanning full width of 2,200 km/s with the approaching and the receding components straddling Sgr A*, each offset from it by 0.11arcsec= 0.004pc. The red-shifted side is displaced to the north-east, while the blue-shifted side is displaced to the south-west. The limit on the total mass of ionized gas estimated from the emission is 10^-4 - 10^-5 Sun at a mean hydrogen density 10^5-10^6 cm^-3, depending upon whether or not we assume the presence of a uniform density disk or an ensemble of orbiting clouds, and the amplification factor of the mm radiation due to the strong background source which is Sgr A* continuum.

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