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Key Facts: RISE Science — Earth Science Exam

ESS.1-ESS.4

Utah SEEd Earth and Space Science strands assessed

Utah SEEd Standards, USBE

4 levels

Proficiency levels reported; no pass/fail cut score

USBE, Making Sense of RISE Scores

Untimed

RISE summative tests are not timed

USBE, RISE Testing: A Guide for Utah Families (June 2026)

$0

Cost to the student for statewide RISE testing

USBE

100

Practice questions in this free OpenExamPrep bank

OpenExamPrep question bank

Utah RISE High School Earth Science is a course-based summative assessment covering the Utah SEEd Earth and Space Science standards (Strands ESS.1-ESS.4). It is computer adaptive, untimed, and free; there is no pass mark, and results report a scale score plus one of four proficiency levels: Level 1 (Below Proficient), Level 2 (Approaching Proficient), Level 3 (Proficient), and Level 4 (Highly Proficient). This bank is an English-language multiple-choice study adaptation. It builds standards knowledge and data interpretation, but it does not replicate the official adaptive delivery, multi-item phenomena clusters, or technology-enhanced modelling tasks.

Sample RISE Science — Earth Science Practice Questions

Try these sample questions to review concepts for the RISE Science — Earth Science exam. Each question includes a detailed explanation. Start the interactive quiz above for the full 100+ question experience with AI tutoring.

1Astrophysicists analyzing cosmic radiation detect a highly uniform microwave signal with a blackbody spectrum corresponding to a temperature of 2.73 Kelvin across all directions of space. Which fundamental theory of space systems does this phenomenon directly support?
A.The Steady State model, showing continuous creation of matter in static space
B.The Big Bang theory, representing relic thermal radiation from the early expanding universe
C.Kepler's Second Law, demonstrating thermal energy conservation in planetary orbits
D.The Nebular Hypothesis, proving solar system accretion from cold interstellar gas
Explanation: The Cosmic Microwave Background (CMB) radiation is thermal remnant radiation emitted roughly 380,000 years after the Big Bang when the universe cooled sufficiently for neutral atoms to form (recombination). Its uniform 2.73 K blackbody profile provides compelling evidence for an expanding, cooling universe that originated from an extremely hot, dense initial state.
2Astronomers observing light from distant galaxies notice that atomic absorption spectral lines are systematically shifted toward longer wavelengths (redshift). According to Hubble's Law, what does a greater redshift indicate about a galaxy?
A.It is moving toward Earth at a high velocity.
B.It contains higher concentrations of heavy metallic elements.
C.It is farther from Earth and receding at a faster velocity due to expanding space.
D.It is approaching the end of its stellar lifecycle as a white dwarf.
Explanation: Hubble's Law ($v = H_0 \cdot d$) demonstrates that the recession velocity of distant galaxies is directly proportional to their distance from Earth. Cosmological redshift occurs because space itself is expanding during light propagation, stretching light waves to longer (redder) wavelengths.
3Measurements of primordial gas clouds in the early universe reveal an elemental mass abundance ratio of approximately 75% hydrogen and 25% helium, with only trace amounts of lithium. Why is this ratio considered major evidence for the Big Bang?
A.Stellar fusion alone would have converted all hydrogen into iron by now.
B.Nuclear synthesis models of the hot, dense early universe accurately predict this exact 3:1 H-to-He ratio.
C.Planetary accretion requires helium to ignite nuclear fission in rocky planet cores.
D.Radioactive decay of heavy uranium naturally yields 75% hydrogen over geologic time.
Explanation: Big Bang Nucleosynthesis (BBN) occurred during the first few minutes after the Big Bang when temperatures and densities were high enough for nuclear fusion. Theoretical physics calculations predict that this process produced approximately 75% hydrogen-1, 25% helium-4, and trace lithium-7, matching observational measurements in unpolluted gas clouds.
4On a Hertzsprung-Russell (H-R) diagram, stars are plotted by surface temperature against luminosity. Where are stable stars that generate energy by fusing hydrogen into helium in their cores located?
A.In the lower-left corner as high-density White Dwarfs
B.In the upper-right corner as low-temperature Supergiants
C.Along a continuous diagonal band known as the Main Sequence
D.Exclusively in the planetary nebula region at the center
Explanation: The Main Sequence is a broad diagonal band on the H-R diagram where stars spend roughly 90% of their lifecycles. All main sequence stars are in hydrostatic equilibrium, fusing hydrogen into helium within their core cores.
5A main sequence star maintains a stable size and structure for billions of years. Which internal equilibrium condition prevents the star from collapsing under its own gravity or expanding uncontrollably?
A.Thermal expansion balancing planetary tidal forces
B.Inward gravitational force balancing outward thermal radiation pressure from nuclear fusion
C.Centrifugal force from rotation balancing magnetic field repulsion
D.Electron degeneracy pressure balancing solar wind ejection
Explanation: Hydrostatic equilibrium in a star occurs when the inward pull of gravity is precisely balanced by the outward thermal radiation pressure generated by core nuclear fusion reactions.
6Kepler's First Law of Planetary Motion reformed astronomical models by describing the geometry of planetary orbits. What shape do planetary orbits follow according to this law?
A.Perfect circles with the Sun located at the exact center
B.Ellipses with the Sun located at one of the two foci
C.Hyperbolas with the Sun located at the vertex
D.Epicycles with the Sun orbiting a central barycenter
Explanation: Kepler's First Law states that every planet moves in an elliptical orbit around the Sun, with the Sun situated at one of the two focal points (foci) of the ellipse.
7In the core of a main-sequence star like our Sun, hydrogen nuclei (protons) fuse to form helium-4 through the proton-proton chain. Why does this nuclear reaction release an immense quantity of energy?
A.The total mass of the resulting helium nucleus is slightly less than the mass of the four original protons, with the missing mass converted into energy ($E=mc^2$).
B.Gravitational potential energy is continuously destroyed as protons collapse into neutrons.
C.Chemical bonds between hydrogen atoms release latent heat during combustion.
D.Neutrinos absorb kinetic energy from space and transfer it into the stellar core.
Explanation: During nuclear fusion ($4 \, ^1\text{H} \rightarrow ^4\text{He} + 2e^+ + 2\nu_e + \gamma$), the mass of one helium-4 nucleus is approximately 0.7% less than the combined mass of four protons. This mass defect ($\Delta m$) is converted into energetic gamma photons according to Einstein's equation $E = \Delta m \cdot c^2$.
8Main sequence stars more massive than about 1.3 solar masses fuse hydrogen into helium primarily via the CNO (Carbon-Nitrogen-Oxygen) cycle rather than the proton-proton chain. What role do carbon, nitrogen, and oxygen nuclei play in this process?
A.They act as nuclear fuel that is permanently consumed to form iron.
B.They act as nuclear catalysts that facilitate proton fusion without being permanently depleted.
C.They absorb thermal energy to cool the core and prevent a supernova explosion.
D.They emit positron radiation to convert the star into a neutron star.
Explanation: In the CNO cycle, carbon-12 nuclei capture protons in a sequence of reactions that yields nitrogen and oxygen isotopes, ultimately releasing a helium-4 nucleus and regenerating the original carbon-12 nucleus. Thus, CNO nuclei function as nuclear catalysts.
9When a low-to-intermediate mass star exhausts its core hydrogen fuel, it expands into a Red Giant. Once the core temperature reaches approximately $10^8 \text{ K}$, what nuclear fusion process ignites in the core?
A.The triple-alpha process, fusing three helium nuclei into carbon-12
B.Silicon burning, fusing silicon into nickel-56
C.Spallation, splitting carbon into lithium and beryllium
D.Proton-proton fusion, fusing deuterium into tritium
Explanation: At core temperatures of $\sim 10^8 \text{ K}$, helium nuclei (alpha particles) overcome electrostatic repulsion. Two alpha particles fuse into unstable beryllium-8, which immediately captures a third alpha particle to form stable carbon-12 ($3\,^4\text{He} \rightarrow ^{12}\text{C}$). This is the triple-alpha process.
10Massive stars ($M > 8 M_\odot$) synthesize progressively heavier elements in concentric nuclear-burning shells around their cores. Why does nucleosynthesis via exothermic fusion halt at iron-56?
A.Iron-56 has the highest nuclear binding energy per nucleon, making fusion of heavier elements endothermic.
B.Iron atoms reflect neutrinos, shutting down all nuclear interactions.
C.The core density drops to zero once iron is produced.
D.Iron nuclei undergo rapid radioactive decay back into hydrogen.
Explanation: Iron-56 (and nickel-56) sits at the peak of the nuclear binding energy curve. Fusing elements lighter than iron releases energy (exothermic), but fusing elements heavier than iron requires net energy input (endothermic). Without energy release to maintain radiation pressure, the core collapses.

About the RISE Science — Earth Science Exam

Master Utah RISE High School Earth Science with 100 phenomena-grounded practice questions structured around Utah SEEd Strands ESS.1 (Matter and Energy in Space), ESS.2 (Patterns in Earth's History and Processes), ESS.3 (System Interactions), and ESS.4 (Stability and Change in Natural Resources).

Exam sponsor: Utah State Board of Education. The requirements and fees below concern the certification or admission exam, separate from our free practice resources.

Assessment

Phenomena-based item clusters, selected-response, and technology-enhanced tasks delivered online through the RISE portal.

Time Limit

Untimed

Passing Score

No pass/fail cut score; results report a scale score plus one of four proficiency levels (Level 3 = Proficient)

Exam / Certification Fees

$0 (state-funded; free for Utah public school students)

Exam sponsor website

Fees, eligibility, and exam policies can change. Confirm them with the exam sponsor before applying or paying.

Our practice resources: topics covered

We aim to reflect publicly available exam outlines and topic information in our study resources. Coverage, format, and difficulty may differ from the actual exam, and we cannot guarantee that every detail is accurate or current. Confirm exam requirements, fees, and policies with the official exam sponsor.

20% of this practice bank

SEEd Strand ESS.1: Matter and Energy in Space

Big Bang evidence including cosmic microwave background radiation and galaxy redshift, stellar evolution on the Hertzsprung-Russell diagram, nucleosynthesis of elements heavier than hydrogen and helium, Kepler's laws governing orbital motion, and radiometric dating of Earth materials and meteorites.

30% of this practice bank

SEEd Strand ESS.2: Patterns in Earth's History and Processes

Mantle convection and heat transport from Earth's core, plate tectonics mechanisms at divergent, convergent, and transform boundaries, subduction zone dynamics, mantle plumes and hotspot volcanism, P and S seismic wave propagation, core shadow zones, and geodynamo generation of the protective magnetosphere.

30% of this practice bank

SEEd Strand ESS.3: System Interactions: Atmosphere, Hydrosphere, and Geosphere

Earth's radiative energy balance (insolation, albedo, and re-radiation), thermal infrared absorption by greenhouse gases, global carbon reservoirs and cycling fluxes, thermohaline and wind-driven ocean circulation, Hadley and Ferrel atmospheric cells, climate positive/negative feedback loops, and paleoclimate proxy records from ice cores and tree rings.

20% of this practice bank

SEEd Strand ESS.4: Stability and Change in Natural Resources

Tectonic and hydrologic processes controlling the uneven geographic distribution of fossil fuels, metallic ores, and groundwater aquifers; engineering principles of renewable energy technologies; coastal erosion and flood mitigation strategies; climate mitigation modeling; and natural hazard risk forecasting.

Preparing for the RISE Science — Earth Science Exam

What You Need to Know

  • Passing score: No pass/fail cut score; results report a scale score plus one of four proficiency levels (Level 3 = Proficient)
  • Assessment: Phenomena-based item clusters, selected-response, and technology-enhanced tasks delivered online through the RISE portal.
  • Time limit: Untimed
  • Exam / certification fees: $0 (state-funded; free for Utah public school students) Official sources

Using Our Practice Resources

  • Work through all 100 available questions
  • Review every answer and explanation
  • Track weak areas and revisit them
  • Use our AI tutor for tough concepts

RISE Science — Earth Science: Suggested Study Strategy

1Master scientific phenomena interpretation by practicing data extraction from graphs of seismic wave velocities, stellar spectrum absorption lines, and ice core isotope ratios.
2Differentiate P-waves (compressional, travel through solids and liquids) from S-waves (shear, travel only through solids) to explain liquid outer core shadow zones.
3Understand the mechanics of Earth's radiative energy balance, including how changes in planetary albedo or greenhouse gas concentrations shift global equilibrium temperature.
4Trace carbon fluxes among atmosphere, ocean, biosphere, and lithosphere reservoirs to identify human impacts on short-term vs long-term carbon cycles.
5Apply Kepler's three laws to predict orbital speed variations at perihelion versus aphelion and calculate planetary orbital periods.

Frequently Asked Questions

What is the Utah RISE Earth Science assessment?

RISE (Readiness, Improvement, Success, and Empowerment) Earth Science is Utah's course-based summative science assessment. Administered by the Utah State Board of Education to students in a RISE-rostered Earth and Space Science course, it measures proficiency on the Utah SEEd (Science with Engineering Education) standards, Strands ESS.1-ESS.4, and is reported independently from the other RISE science course tests.

How are scores and proficiency levels reported on RISE Earth Science?

There is no pass or fail mark. Students receive a scale score plus one of four proficiency levels established by USBE: Level 1 (Below Proficient), Level 2 (Approaching Proficient), Level 3 (Proficient), and Level 4 (Highly Proficient). Reports also break performance down by reporting category.

What topics are covered on the RISE High School Earth Science test?

The four Utah SEEd Earth and Space Science strands: ESS.1 Matter and Energy in Space, ESS.2 Patterns in Earth's History and Processes, ESS.3 System Interactions (Atmosphere, Hydrosphere, and Geosphere), and ESS.4 Stability and Change in Natural Resources. The SEEd science assessment is matrix designed, so an individual student is assessed on a subset of standards within each strand.

How long is the RISE Earth Science test and what does it cost?

RISE assessments are not timed, and there is no fee. RISE is state-funded testing for Utah public and charter school students. For 2026-27, the grades 9-10 science summative window runs March 9 to May 14, 2027.

How does this practice question bank relate to the official RISE exam format?

This is an English-language multiple-choice study adaptation, not an official practice test. The official assessment is computer adaptive and uses phenomena-based item clusters and technology-enhanced tasks. Standalone multiple-choice items build the underlying standards knowledge and data-interpretation skill, but they do not reproduce the official format. Use the free training tests on the Utah RISE portal to practise the real interface.